Desperation grows in battered Honduras, fueling migration – PBS NewsHour

SAN PEDRO SULA, Honduras (AP) Nory Yamileth Hernndez and her three teenage children have been living in a battered tent under a bridge on the outskirts of San Pedro Sula since Hurricane Eta flooded their home in November.

They were there in the dust under the rumbling traffic, surrounded by other storm refugees, when Hurricane Iota hit barely two weeks later. And when the first migrant caravan of the year shuffled by in January, only fear and empty pockets kept them from joining Honduras growing exodus.

I cried because I dont want to be here anymore, the 34-year-old Hernndez said. She had joined the first big caravan in October 2018, but didnt make it to Mexico before turning back. Shes sure she will try again soon. Theres a lot of suffering.

WATCH: Biden rolls back Trumps immigration policies with a raft of initiatives

In San Pedro Sula, Honduras economic engine and the departure gate for thousands of Honduran migrants in recent years, families like Hernndezs are caught in a cycle of migration. Poverty and gang violence push them out and increasingly aggressive measures to stop them, driven by the United States government, scuttle their efforts and send them back.

The economic damage of the COVID-19 pandemic and the devastation wrought by Novembers hurricanes have only added to those driving forces. Word of a new administration in the U.S. with a softer approach to migrants has raised hopes, too.

After her failed attempt to migrate in 2018, Hernndez returned to scraping out a living in San Pedro Sula. Last year, she sold lingerie door-to-door in one of the countrys most dangerous neighborhoods. But the storms wiped out her inventory and her customers had limited ability to pay her for items they bought on credit.

I couldnt charge people because we all lost, Hernndez said. We all have needs, but you have to be sensitive. They dont have anything to pay with and why go to collect?

Chamelecon is a neighborhood of low, tin-roofed houses and small shops with barred windows on the outskirts of the city. Only two of its streets are paved, including one that is the dividing line between the rival gangs Mara Salvatrucha and Barrio 18.

At the bridge where Hernndezs tent is pitched, tattooed youths smoke marijuana and residents slop around in rubber boots. The violence continues, with newspapers talking about finding bodies wrapped in plastic.

In December, Hernndez got sick with fever, nausea and, she said, her brain hurt. She went to a hospital, but was never tested for COVID-19. In January, her eldest son writhed in their tent with fever.

The father of her youngest son lives in Los Angeles and encouraged her to get money together for another trip. He told me that this year is going to be good because they had gotten rid of Trump and the new president was going to help migrants, Hernndez said.

Within weeks, U.S. President Joe Biden signed nine executive orders reversing Trump measures related to family separation, border security and immigration. But fearing a surge in immigration, the administration also sent the message that little will change quickly for migrants arriving at the southern U.S. border.

Hernndez recently found work cleaning flooded streets, but she still hasnt been able to tackle the house where she once lived with 11 others. Its still filled with several inches of mud and foul water.

The assembly plants that surround San Pedro Sula and power its economy are still not back to pre-hurricane capacity amid the pandemic.

The Sula Valley, Honduras most agriculturally productive, was so heavily damaged that international organizations have warned of a food crisis. The World Food Program says 3 million Hondurans face food insecurity, six times higher than before. The dual hurricanes affected an estimated 4 million of Honduras 10 million people. The area is also Honduras hardest-hit by COVID-19 infections.

Its a vicious cycle, said Dana Graber Ladek, head of the International Organization for Migration office in Mexico. Theyre suffering poverty, violence, the hurricanes, unemployment, domestic violence, and with that dream of a new (U.S.) administration, of new opportunities, theyre going to try (to migrate) again and again.

The last several attempted caravans have been foiled, first in Mexico and later in Guatemala, but the daily flow of migrants moved by smugglers continues and has shown signs of increasing. The hope and misinformation associated with the new U.S. administration helps that business too.

The traffickers are using this opportunity of desperation, of political changes in the United States to spread rumors and false information, Graber Ladek said.

In January, San Pedro Sula was abuzz with plans to migrate.

READ MORE: DOJ rescinds zero tolerance immigration rule

Gabriela, 29, feeling like she had nothing to lose, went north just days before a few thousand Hondurans headed out of San Pedro Sula on Jan. 15. She had lost her cleaning job in the pandemic and the rest of her life to the hurricanes. She asked that her full name be withheld because she had made it to southern Mexico and feared being targeted.

Gabriela paid a smuggler, paid off authorities along her route and walked through jungle as part of her journey north.

She had lived in La Lima, a suburb of San Pedro Sula. Small businesses there have begun to reopen, but in outlying neighborhoods, the streets are still full of debris, dead animals, snakes and burning mattresses.

Everyone wanted to leave, said Juan Antonio Ramrez, an elderly resident. His children and grandchildren were among some 30 people who spent six days stranded on a corrugated metal roof surrounded by floodwaters in November. A lot of people went from here, but they all came back. The problem is theres a barrier and they send them back from Guatemala.

After the 2018 caravans and rising number of migrants at the U.S. border in early 2019, the U.S. government pressured Mexico and Central American countries to do more to slow migration across their territories. Numbers fell in the latter half of 2019 and Mexico and Guatemala effectively stopped caravans in 2020. In December, a caravan leaving San Pedro Sula didnt even make it out of Honduras.

But the U.S. has reported a rising number of encounters at the border, showing that beyond the caravans, the migration flow is increasing again.

In September, Lisethe Contreras husband made it to Miami. The La Lima resident said it took him three months and $12,000 paid to smugglers. Shes thinking of going too, but for the moment has her small business selling necessities.

Biden has promised investment in Central America to get at the root causes of immigration, but no one expects to see any change soon. Honduras primary elections are scheduled for March and nongovernmental organizations worry any aid will come with political strings attached.

Hernndez admits confusion and disillusion. I dont know. They all promise and then dont follow through, she said. I dont see a good future here.

Gabriela, already halfway to her goal of reaching the U.S., has no thoughts of turning back, even after 19 people, believed to be mostly Guatemalan migrants, were found shot and burned in northern Mexico just across from Texas.

I only go back to Honduras if Immigration sends me back, she said. And if that happens Ill try again with my son.

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Desperation grows in battered Honduras, fueling migration - PBS NewsHour

How the UK is headed for a perfect storm on human trafficking, according to author of The Truth About Modern Slavery – St Helens Reporter

That is according to Emily Kenway, author of The Truth About Modern Slavery, published in January.

Drawing on professional experience, plus conversations with senior police officers, campaigners and victims, Kenway takes a closer look at the reality behind the headlines and government rhetoric on this issue. She presents a troubling picture.

Kenway served as an advisor to the first Independent Anti-slavery Commissioner, Kevin Hyland, a role created by the 2015 Modern Slavery Act. Shes worked specifically on modern slavery, but, she stresses, shes also been involved with issues which relate and feed into it.

This is one of the main things Kenway hopes her readers take to tackle the issue of modern slavery, we have to see it in a societal context and understand what makes it possible.

The main drivers behind this are poverty, insecure immigration status, a context where labour rights have been gradually eroded, Kenway told JPI Media. All these things create opportunities for people to be exploited.

Kenway had begun work on the book when, in October 2019, news broke that a number of people had been found dead in the back of a lorry in Essex.

The reaction from some politicians, she says, perfectly illustrated one of her core criticisms of how modern slavery is understood.

The local MP and Priti Patel were referring to this as related to trafficking. But I knew they couldn't possibly know that because it was only a few hours after they'd been discovered, she said.

This is how trafficking as a part of modern slavery is used to make the public misunderstand what's actually going on. They are doing so because the public immediately then thinks of the traffickers as the perpetrators, we think of these individual deviants who have caused these horrific deaths.

When the case did eventually go to trial it was as a case of migrant smuggling, which is a different issue to human trafficking, explains Kenway.

If instead we understand it as a case of migrant smuggling, we have to ask why people are risking losing their lives in order to get to other countries and that becomes a question of borders and governance, she said.

Kenway argues that these same hypocrises exist in other aspects of the Governments approach to modern slavery. She highlights numerous cases where senior police figures announced raids on sex workers under the banner of human trafficking operations.

After looking in depth at these operations and the outcomes, Kenway discovered that women were often arrested, but very few if any referrals were made to the the modern slavery pathway, the National Referral Mechanism.

Kenway also points to some of the requirements of the Modern Slavery Act as being wholly inadequate, such as the stipulation that large firms publish statements about their supply chains.

A company could write a statement which says We have done nothing about modern slavery, and effectively, that would comply with the law, she says.

This means firms which go the extra mile to make sure their supply chains are not party to exploitation such as stone-firm Marshalls, cited throughout the book as an example of a firm getting it right are at a disadvantage to those which pay no heed to the issue.

Kenway is not optimistic about the future of modern slavery. Indeed, she says, we may actually be headed for a perfect storm.

A migration crisis driven by climate breakdown, the post-Covid economic shock and Brexit - which will create another group of people who are undocumented, and may likely lead to a reduction in labour rights - mean this is only going to get worse, she says.

Unless we change the way we think about and approach these issues, there are going to be millions of people suffering these kinds of exploitation.

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How the UK is headed for a perfect storm on human trafficking, according to author of The Truth About Modern Slavery - St Helens Reporter

Lebanon: Overlapping crises exacerbate medical needs and worsen access to care – Doctors Without Borders

Since the explosion, the public health system has also struggled to cope with the growing number of COVID-19 cases, which rose from less than 200 cases a day before the blast to an average of 1,500 in December 2020. To date, more than 226,000 cases have been reported nationwide.

In August 2020, MSF stepped up efforts to respond to COVID-19 in Lebanon and support the national health system in dealing with the pandemic. We temporarily turned our hospital in Bar Elias, in the Bekaa Valley, into a COVID-19 facility and now support an isolation center in Sibline, in the south of the country. MSF teams are also involved in testing, health promotion, and training activities in different locations across the country. Lockdown measures, although necessary, have worsened peoples economic difficulties.

My husband used to find daily laborer jobs in agriculture or construction, said Samaher, a 40-year-old Syrian refugee who lives in an informal tented settlement in Akkar governorate, near the Syrian border. But with the economic situation and the coronavirus, it has become more difficult. He only works two or three days a week, and sometimes theres no work for [two weeks]. When he doesnt find work, we have to borrow money from the neighbors so we can buy food.

For many people in Lebanon, whether they are Lebanese, refugees, or migrant workers, the current economic crisis and the deteriorating living conditions come on top of other traumatic events and stressful experiences, such as conflict or displacement, disrupting psychological wellbeing. Many patients who request MSFs mental health services in Lebanon show symptoms related to emotional distress, depression, anxiety, and hopelessness.

I feel completely down and useless. The economic situation in the country is a disaster. I only hope we wont end up in the streets, said Tawfik, a Palestinian refugee living in Shatila camp in Beirut. His family relies entirely on UN agencies and nongovernmental organizations to survive. We are so tired, adds Hanadi, his wife, unable to hold back her tears while she speaks.

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Lebanon: Overlapping crises exacerbate medical needs and worsen access to care - Doctors Without Borders

Empowering the Migrants: Requisites and Rationalities | Nupur (…) – Mainstream – Mainstream

Home > 2021 > Empowering the Migrants: Requisites and Rationalities | Nupur(...)

by Nupur Pattanaik

The paper analyses the plight of migrants and talks about the atrocities encountered by the migrant community during the pandemic. The Covid-19 has brought to the spotlight the trials and tribulations faced by women, children, old aged people in the pandemic and how they have been succumbing to exploitation and marginalisation, the need for efficient paradigms and perspectives to make migration safer and needed for the development of the nation. It reflects a need for rational and emergent mechanisms to pave way for better capability and empowerment schemes to elevate the migrant communities by the inclusion of women, children-base entitlements and make migration feasible and safe in the Post-Covid Times for their upliftment and advancement, making migration governance the new normal implications and the order in the new Covid-free world.

Locking and Unlocking in India due to the universal pandemic has highlighted the major paradigms of the migrant plight, the economic halt and situated the conditions of the migrant workers. Invisible, unrecognised vulnerabilities pre-locking and post-unlocking of the nation confronted by the migrant masses has some-way or the other has overblown them. Migrant workers are the spine of Indias informal sector, their movement to states jobs indicates economic integration, and also inter-regional and rural-urban disparities. While empowering themselves, they also enrich their home and host regions. The national lockdown due to the corona-virus contagion has threatened and unravelled the phenomena of migrant crisis; Their mass exodus from the places has created a humanitarian and health, security confrontations, and a logistical nightmare. A Report by World Economic Forum exposes the existing problems, and a need for urban reforms as the pandemic has affected the migrants and post-pandemic there would be imbalances, inequalities, oppressions, disparities towards the poor-low income groups especially the migrants. Remittances are much lower than the Pre-Covid days which have affected their livelihood. Economic precarity, lack of adequate shelter, infections and inadequacy of protective gear, lack of basic services has been a way of life for the migrants. The challenges of the Covid-19 pandemic in India particularly on the migrants internal international diasporic communities and refugees irrespective of their status and has drastically contrived their human rights.

Every year The International Day of Migrants celebrated on 18th December. The year 2020 was a year of massive pretentious trouble for them and the refugees and migrants were remembered who have lost their lives, the major theme was to reimagine human mobility. Migration is a process and not a problem, it is for better livelihood and should not be seen as a suffering trend, but due to a lack of effective well-timed safety measures, they have encountered adversities and misfortunes. Ellsworth Huntington, an eminent geographer who opined that History in its most comprehensive and inclusive aspect is a record of human beings migrations from one environment to another. Globally the enormity of migrant crisis has been exposed by the pandemic like never before. The struggle and strain confronted by migrants are of inconceivable forms. The media visuals of millions of migrant workers out on the road, when the sudden lockdown was first announced in India in the last week of March is still afresh among the masses.

According to a report by The Global Migration data portal reveals that the number of global migrants or people living in a country of destination other than their country of origin in 2019 had reached 272 million, Women migrants account for 48 per cent of the total number, 38 million are the child population, Three out of four international migrants are depicted of the working-age, that is between 20 and 64, It has been estimated that 31 per cent of the international migrants worldwide are in Asia, 30 per cent in Europe, 26 per cent in the Americas, 10 per cent in Africa and three per cent in Oceanian countries.

Lives and Livelihood

Migration has been shaping our world in every turn, in an era of deepening globalization, increased digitalization and rapid urbanization, migration touches all States and people more than ever before. Migration is an expression of development, the inclusion of migration in the 2030 Agenda for Sustainable Development presents a glorious platform to estimate the impact of migration on a range of development issues and to understand better how development can impact on migration and migrants. The central theme to migration in the 2030 Agenda is to Reduce inequality in and among countries. It has been a mechanism for orderly safe regular and responsible migration and movement of people through the implementation of planned and well-managed policies for migrant communities.

The epoch of Pandemic and the post-pandemic world has brought a threat to their lives and livelihood which has positioned them in a deplorable condition. The pandemic has disproportionately affected them and made them marginalised. They have become the victims of violence, atrocities, trafficking and many forms of social maladies, basically, children of these migrants too suffered, and also they had become the sufferer of gender inequalities. Women migrant workers are often employed in domestic work, and many of them have suddenly lost their jobs because employers perceive them as carriers of the infected virus. Those who are employed in hospitals, and care sectors like health care clinics and old-age care facilities, looking after COVID-19 masses or cleaning hospital rooms, putting their lives to risk on a daily basis. In addition, women migrant workers who are pushed into the margins of society during the catastrophe are likely to experience the enormous intensity of marginality, harassment and violence. With services such as emergency hotline services being less active due to the universal pandemic, they will have lesser ways to get help services and escape it.

The Covid-19 activated mass migration which is a sudden reversal of this cumulative migration of seven decades, since the partition of India when 14.5 million people migrated. The pandemic has worsened their lives and right to live and a threat to their physical and social well-being. Around 30% of immigrants live in relative poverty in the OECD (Organisation for Economic Co-operation and Development), compared with 20% of the native-born (OECD/European Union, They are also more likely to live in sub-standard accommodations (23% against 19%) and twice as likely in overcrowded dwellings (17% against 8%). Lack of basic conditions has increased the likeliness of infection, especially given that immigrants are more likely to live in extended cohabiting families.

The pandemic extremed the violence against women migrants specifically domestic maids, children, old aged migrants by the domestic violence, child marriage issues due to utmost poverty, trafficking trade of women migrants were some of the dark sides of the pandemic. Child Abuse, Exploitation, foeticide, stigmatisation were some of the noted phenomena witnessed during the times and there is a need to give a rethought to change their situations and circumstances and prepare them to be capable and enlightened so they can be an active contributor for their own livelihoods and development of nation in the coming times.

The pandemic has significantly escalated their plight. The travails and travesties of these workers need to be addressed, though policies and programmes have been there but a needed deeper level analysis to contribute for their mental well-being is required. A migrant worker from Koraput, Odisha voiced on anonymity that due to pandemic and post-pandemic work responsibilities he has been witnessing ostracizations, xenophobia and stigmatisation from the people around the place of work, a domestic women migrant worker from the same place was jobless due to the pandemic and opined that she has been a victim of domestic violence as she was not having an income.

Empowerment and Entitlements

From hardship to hope for the migrants, the need for migration governance, by achieving human rights and gender rights and organising them for their rights and responsibilities is a needed rational requirement, acting with a sense of urgency is a prerequisite to cater their needs and preparing them for a post-covid world order. Empowerment in the migration process can specifically allow the migrant communities to make right and active choices and protect them from pressure and excessive influence by others in their community of origin and after migration and prevent themselves from every aspect of discrimination. However, the conditions that allow these migrants irrespective of caste, class, faith and gender divide to assert their power and achieve them. Women migrants though constitute a majority of international migrants and should be entitled with rights and several benefits are not somehow incorporated in the gender dimension of migration. The multidimensional aspects of gender, migration and empowerment should be dealt from a multi-pronged perspective. The constraints and enablers, the empowerment and disempowerment processes should be taken into consideration to frame out better and effective policies and privileges in the Post-Covid world order.

While human mobility has been an essential feature of our global history, it is as pertinent today as it ever was in the past. It has been estimated by recent calculus released by the United Nations Department of Economic and Social Affairs (UNDESA) that 232 million international migrants in the world, migration is and always has been one of the most significant and pressing global issues of the times. The economic, social, and civic proportions of integration needed to be addressed comprehensively. Encouraging migration for better development is a needed recipe for the hour as the pandemic has retrenched and reshuffled the desire for migration. The emergent adequacy to entitle the migrant community should be the outlook to promote mobility and migration. The role of civil society, NGOs (Non-Governmental Organisation), Media and other positive communities should play a priority role in encouraging safe migration.

Rethinking mobility and migration strategies, migrant inclusivity, a new urban paradigm to prepare for a post-pandemic world through various policy frameworks should be introduced for uplifting the migrant communities, the parameters of empowerment should be relocated to usher in an equal safe haven for the migrants.

References

1.https://www.ndtv.com/india-news/international-migrants-day-2020-key-facts-on-global-migrant-crisis-23400592.https://economictimes.indiatimes.com/news/economy/policy/view-india-should-use-migrant-labour-crisis-to-transform-economy-society/articleshow/76184723.cms3.https://www.who.int/news-room/feature-stories/detail/migrants-and-refugees-say-covid-19-has-dramatically-worsened-their-lives4.https://www.oecd.org/coronavirus/policy-responses/what-is-the-impact-of-the-covid-19-pandemic-on-immigrants-and-their-children-e7cbb7de/5.https://www.unescap.org/blog/plight-migrants-under-spotlight-covid-19-responses6. https://www.iom.int/

(Author: Dr Nupur Pattanaik is associated with the Department of Sociology, Central University of Odisha)

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Empowering the Migrants: Requisites and Rationalities | Nupur (...) - Mainstream - Mainstream

The 25th anniversary of Deep Blue beating Garry Kasparov in a chess game. – Slate

Chess has captured the imagination of humans for centuries due to its strategic beautyan objective, board-based testament to the power of mortal intuition. Twenty-five years ago Wednesday, though, human superiority on a chessboard was seriously threatened for the first time.

At a nondescript convention center in Philadelphia, a meticulously constructed supercomputer called Deep Blue faced off against Garry Kasparov for the first in a series of six games. Kasparov was world chess champion at the time and widely considered to be one of the greatest players in the history of chess. He did not expect to lose. It was perhaps understandable; 1996 was an age of fairly primitive computer beings. Personal computers were only just becoming a more affordable commodity (35 percent of U.S. households owned a computer in 1997, compared with 15 percent in 1990), the USB had just been released, and it would be another five years until Windows XP made its way onto the market.

But Deep Blue was no run-of-the-mill computer. It was a behemoth built with the sole intention of being very good at chess. And it fulfilled that mission. On Feb. 10, 1996, the reigning world chess champion lost a game to a computer for the first time in history. Kasparov would win the 1996 match four games to two, but in May 1997, an upgraded Deep Blue would defeat Kasparov 32.

The 96 match nonetheless demonstrated that the tide was starting to turn in the chess world, and the tide was deep, blue, and electronic. It introduced chess computers to the world, sparking conversations about a rise of automation in the famously romantic field.

Some version of computers had been playing chess even before the emergence of artificial intelligence as an official field in the 1950s. Alan Turing, the famous cryptographer, had developed a handwritten chess algorithm in 1950 called Turochamp. In 1957, Alex Bernstein, a researcher and chess enthusiast from the Bronx, created the first complete chess program with the help of a number of his IBM colleagues.

Computer chess changed in the 80s. says Jonathan Schaeffer, president of the International Computer Games Association and professor of computer science at the University of Alberta. That decade, pioneering American computer scientist Ken Thompson released a paper proving something that now seems intuitive: If your computer was faster, your chess program would perform better. Programs could thus analyze more and more moves per second, increasing their chances of finding the best move possible.

Accordingly, computer chess became about getting the fastest technology. When I started in the [computer chess] game, we were using a single computer. Then it became 16, then 210, and so on to chips and supercomputers, says Schaeffer. In 1988, students at Carnegie Mellon University developed a sophisticated chess computer called Deep Thought. In January of that year, Deep Thought became the first computer to beat a grandmaster in a regular tournament game when it triumphed over Bent Larsen, a Danish GM. The next year, IBM hired three of those Carnegie students, Feng-hsiung Hsu, Thomas Anantharaman, and Murray Campbell, with the express aim of building a chess computer to rival the world champion; they would be joined by Chung Jen-Tan, Joseph Hoane Jr., and Jerry Brody later in the project. In October 1989, Kasparov played two games against Deep Thought, winning both of them with ease.

The first match demonstrated that the tide was starting to turn in the chessworld.

The loss to Kasparov in 1989 demonstrated the amount of work that needed to be done, says Schaeffer, so they took it to the extreme. They went off for seven years and built new computer chips that were faster, building a system that was scaled up to not just four computer chips, but 500. They added more knowledge to it as well as a book of openings, and eventually the brain of chess grandmaster Joel Benjamin helped provide expertise. This was a very long project involving many, many people, and significant financial expense, but it paid off for IBM in the form of media clamor.

The 2,800-pound Deep Blue, complete with special-purpose chess computer chips, was the end product. It was capable of processing 200 million moves per second, or 199,999,997 more than Kasparov could manage, according to IBM. This produced a chess machine that was stronger than any of its automated predecessors, and the outside world was stunned at the eventual resulta human had been outdone by a machine in this game of intellect, wit, and judgment. At the 1997 match, Kasparov and Deep Blue would go toe-to-automated-toe in front of numerous television cameras and a large crowd.

But Kasparovs loss was not as devastating as casual observers might have expected. Computers had beaten grandmasters before; it was inevitable that someone of Kasparovs stature would fall too. And though Kasparovs loss certainly came earlier than expected, the competitive chess world continued to go about its business relatively unfettered.

I dont think it affected chess players too much, says Matthew Sadler, chess grandmaster and co-author of Game Changer, a book about modern chess engine AlphaZero, Firstly, Kasparov was probably stronger than Deep Blue at the time, despite the loss. Secondly, it didnt really inspire any chess players with its play.

It helped that Deep Blue, at the time, was the exception rather than the rulemachines of its strength werent widely available. In 2006, though, a chess computer called Deep Fritz beat thenworld champion Vladimir Kramnik. I think thats really when chess players sort of thought, Oh, my goodness, the machines really are getting stronger than us, says Sadler, when they were beating us not on supercomputers, but on relative commodity hardware.

The change here wasnt just that a computer could win, but that a computer could help human players win if incorporated into their training regimes effectively. Computers were adept at judging the quality of moves and positions accurately, particularly during opening sequences. Some found this easier than others. Sadler says: I think a lot of competitive players took a while to adjust to the new reality. For example, if you werent really computer-literate, and all of a sudden you found yourself in a world where having a computer really makes a difference, thats a difficult thing.

Despite initial resistance from certain parts of the community, the advantages that computers afforded chess players eventually made them impossible to ignore. Sam Shankland gained his international master title in 2008, right around when computers started to become a necessity. There was some backlash, but honestly, those people are mostly gone now, Shankland, now a grandmaster and 2018 U.S. chess champion, says. They either got tired of losing and quit chess or they got tired of losing and adapted.

The sheer wealth of knowledge chess players now had access to meant that determination was increasingly rewarded. I think that chess is essentially a subset of talent and hard work, says Shankland, and as training resources like computers become better and more accessible, talent tends to become less important compared to hard workwhich suits a workhorse like myself.

Such accessibility has also led to chess, once reserved for rich families who could afford tutors and other training, to become a markedly more democratized pursuit. Take India, for example, says Shankland. Apart from Vishy [Anand], they werent a particularly strong chess nation historically. Now, theyre clearly the fastest-growing country in the world in terms of rising stars, and I think a lot of that is down to training resources becoming more widely available.

The availability of advanced chess analysis at the flick of a smartphone has caused a bizarre balance of power in the media and a certain trepidation among top-level players, as Peter Heine Nielsen, coach of current world champion Magnus Carlsen, points out:

When I started working with Vishy Anand, at a postgame press conference the players would explain the games, and everybody would look at them with excitement and think, Wow, these guys are clever. Now, the player in the press conference is a bit nervous because they have only calculated themselves, while all the journalists have been using advanced technology. So they are afraid to say, I thought this wasnt a strong move in case theyre wrong.

So sometimes before a press conference I speak to Magnus and tell him the computer said this or that, just so he knows. The spectator-player dynamic has changed a lotsome of the mystery has gone.

However, while certain human aspects of the games have disappeared, recent developments have caused professional players to rethink what they know about their beloved board game. In 2017, a team of scientists at Google-owned DeepMind created AlphaZero, a self-learning neural network program that surpassed the strongest chess program after just four hours of playing against itself.

Before the computer boom, and before the neural network boom, we were thinking quite dogmatically, says Nielsen. After both occurred, we were forced to rewrite our own solutions. It led to the game becoming more exciting. Moreover, the two strongest chess enginesLeela (which is based on AlphaZero) and Stockfishare available online, which signifies a remarkably more distributive and collaborative approach to chess innovation than that which was pioneered by Deep Blue, a closed circuit.

Despite all their progress, there are still some goals to which innovators in the chess world can aspire. The next step is for engines to explain what theyre doing, says Sadler, so that the average player can understand why an engine says, No, trading that piece is a bad idea. The relationship remains one of reciprocity.

One thing is certain: Chess programs will remain the most important piece of a professional players preparatory arsenal. Not using a computer to do chess would be like not using a calculator to do math, says Nielsen, I like itbut it doesnt matter if I like it or not. Its the right way to do it.

Future Tense is a partnership of Slate, New America, and Arizona State University that examines emerging technologies, public policy, and society.

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The 25th anniversary of Deep Blue beating Garry Kasparov in a chess game. - Slate

Fat Fritz 2: The Best of Both Worlds – Chessbase News

It has been an extraordinary year for everyone, but no less so in computer chess. You would be forgiven for thinking we had seen the last major revolution in the field, thanks to AlphaZero and all the works it inspired and spawned. The neural network technology they created was staggering and incredible, and while it is still being explored and worked on, a new development has come to the chess world thanks to chesss Japanese sibling, Shogi.

Although the AlphaZero neural network is extremely powerful overall, and consequently Leela and Fat Fritz, it is held back by the need to use a GPU (graphics processor) to read it, slowing it down by over a thousand times compared to traditional speed demons such as Stockfish and Komodo. That it could still compete with them on equal terms in spite of this handicap speaks volumes on just how powerful those neural networks are.

Still, this came at a price too. The nature of its search, averaging the various outcomes, good or bad, led to a strongly exploitative style, but could fail in technical endgames or positions where surgical precision was needed. The dream of combining a large and powerful neural network with the speed and accuracy of Stockfishs search seemed just that: a dream.

Enter NNUE.

As chess players we naturally think of AlphaZero as a chess engine development first and foremost, whilst acknowledgingGo was its originator. It is easy to forget that the AlphaZero paper described its applications to three strategy games, not two, the third being the Japanese chess game known as Shogi.

Unsurprisingly, the shogi world was no less shaken up by the AlphaZero paper, but instead of just trying to reproduce it, a Japanese programmer, Yu Nasu, developed and published agroundbreaking paperfora different neural network architecture known as NNUE, inspired by DeepMinds success, whichran at full strength exclusively ona computer processor with no need for avideo card.

Just asAlphaZero and the first edition of Fat Fritz, NNUEalso builds it own chess knowledge by learning from chess positions and evaluations. NNUE completely revolutionized Shogi programs, leading to leaps of well over 100 Elo!It was their developers who shared their work with the chess world by adapting their open source Shogi NNUE code to the open source programStockfish. Based on the success of Stockfish 12, the first chess engine to implement NNUE, numerous other engine authors have also added NNUE into their work, such as the recently released "Dragon" by the Komodo team.

Order Fat Fritz 2 in the ChessBase Shop now

Fat Fritz 2 is trained and developed using this NNUE technology, runninginside the open source Stockfish binary, butwith a completely new and different neural network that differs significantly from Stockfish's on a couple of key points:

After all, if an elite neural network could be trained from just Stockfish evaluations, imagine what it could do with the sophisticated knowledge of Fat Fritz!To this end, some four billion positions were generated on thousands of hours of the most powerful graphics cards to train it.

So what was the result of this larger neural network with deeper chess knowledge?Ina large test at 1 minuteplus 1 second, Fat Fritz 2 scored +42 Elo over Stockfish 12.Click to download the PGN games.

Score of Fat Fritz 2 vs Stockfish 12:

286 wins / 99 losses /1167 draws

Elo difference: 42.1 +/- 8.5, LOS: 100.0 %, DrawRatio: 75.2 %1552 of 1552 games finished.

Note: the reason for the odd number of games is that the suite used has 776 positions, which with reversed colours leads to 1552games.

Also, there is reason to believe that its endgame play is superior overall, though even if true, exceptions will no doubt be found. Here are a few examples:

This has often been a very tough one for engines, even when enjoying all the tablebases available. Using a modest sixcores to emulate laptop users or those with less than premium desktops, here are the results of Stockfish 12 and Fat Fritz 2:

Analysis by Stockfish 12

While taking 37 seconds might not seem like a big deal, most people will not spend that long with an engine on a position unless they already suspect there might be something to uncover.

Analysis by Fat Fritz 2

Five seconds! True, this is but a single position, yet there is a reason Shirov's move remains in modern test sets to this day.

Another curiosity actually comes from an article published a few months ago by GM Karsten Mueller. He had asked for the analysis of a development version of Fat Fritz 2, and in itone of his moves had been refuted badly... much to his delight. The reason for his pleasure was that it showed new engines might become even more valuable tools in complex endgames.

Here Fat Fritz 2gave a winningline starting with 52...e7.

This same position was then shown to Stockfish 12, which had access to 30 threads, 7-piece tablebases, and after nine billion nodes it declared 52.d6 was winning and its choice.

There doesn't seem to be much doubt with such a high evaluation, does there?

Was this a case of more than one move doing the job? 52.d6 was then shown to Fat Fritz 2, but it declared this move and line a draw! According to it,there was a blunder just five plies into Stockfish's 50-ply mainline.

Instead of 56.h3? as shown above, Fat Fritz 2's 56.Nb4! saves the game. Granted, none of this is absolute proof, but this sort of thing has been common enough to stand out.

Regardless, it is clear Fat Fritz 2 is an enormous step forward, and will offer fantastic analysis and pleasure to all who use it. Anyone who felt left out, due to the previous need to use a powerful video card to reap the benefits of a world-class neural network, can now rejoice asthis is no longer required.

Order Fat Fritz 2 in the ChessBase Shop now(best by download, to get it immediately)

No such work is the result of one person, whether directly or indirectly, and this is no less true of Fat Fritz 2.

Deepest thanks and gratitude go to my friend Daniel Uranga, a brilliant Argentinian programmer who helped realize and test every mad idea I came up with, and there were many. His help was invaluable and his skill has now been deservedly recognized by Amazon who recently hired him and brought him to the UK.

Also, warmest thanks to my friend Dietrich Kappe who is an endless source of useful scripts and ideas, and who helped take the project to the next level. His friendship and generosity cannot be overstated.

Finally, where would any of this be without the fabulous Stockfish team and their legion of contributors, as well as Yu Nasu for his groundbreaking NNUE work, and Tanuki (nodchip) for his translation of the Shogi code for use in chess.

Originally posted here:

Fat Fritz 2: The Best of Both Worlds - Chessbase News

Fat Fritz 2.0 – The new number 1 – Chessbase News

Fat Fritz has revolutionised the world of chess engines. The AI engine is based on the famous AlphaZero algorithms: the extraordinary playing strength and the completely new analyses fascinated the chess world. Now Fat Fritz 2.0 has arrived!

Fat Fritz 2.0 is based on the Stockfish 12 engine, but uses a completely new neural network with better ratings and greater performance.

NNUE-Technology:

Fat Fritz 2.0 achieves top performance even without a high-end graphics card!

Fat Fritz 2.0 miles ahead!

In the comparative match over 1552 games Fat Fritz 2.0 clearly beats Stockfish 12 (286 wins with 99 losses, rest draws) and outperforms the previous top engine by over 40 Elo points (as of February 2021).

Incl. Fritz 17 user interface (64 Bit).

Runs on any current Windows PC or laptop.

What you receive:

ChessBase Premium-Membership (sixmonths) with access to the ChessBase Video Portal, Playchess, the Tactic-App, LiveDatabase, LiveBook etc. Database of around 1.5 Mio. Games, and much more

Order Fat Fritz 2 in the ChessBase Shop now(best by download, to get it immediately)

Or: how about trying it out on our engine cloud?

SYSTEM REQUIREMENTS:

Minimum: PC Core i3 or i5 / AMD FX or Ryzen 3, 2 GB RAM, Windows 7/8/8.1 64Bit, DirectX9, graphics card with 256 MB RAM, DVD-ROM drive, Windows Media Player 11 and Internet access.

Recommended: PC Core i7, i9 or AMD FX, Ryzen 7/9 and Windows 10 64-Bit, 4 GB RAM, Windows 10, DirectX10, graphics card with 512 MB RAM or more, Windows Media Player 11, DVD ROM drive and Internet access. System requirements for ChessBase Account: Internet access and up-to-date browser, e.g. Chrome, Safari. Runs on Windows, OS X, iOS, Android and Linux.

See the article here:

Fat Fritz 2.0 - The new number 1 - Chessbase News

FINAL DEADLINE: FIRST FILING AND TOP RANKED LAW FIRM, Encourages Sona Nanotech Inc. Investors with Large Losses to Secure Counsel Before Important…

TipRanks

We are indeed living in interesting times and in many ways, thats a good thing. Take the automotive industry, for example. Technology is changing a rapid pace, and when it settles, it will dramatically change the way we drive. In 2030, our concept of car will likely be unrecognizable to drivers from 1980. The biggest changes are coming from power systems and artificial intelligence. AI will bring autonomous tech to our cars, making self-driving vehicles a reality. But the power systems changes will hit us first. In fact, electric-drive vehicles are already on our roads, and electric vehicle (EV) companies are proliferating rapidly. For the moment, there are several roads to potential success in the EV market. Companies are working to position themselves as leaders in battery tech, or electric power trains, or to maximize their range and performance per charge. Its a fact-paced industry environment, offering both opportunity and excitement for investors. Smart investors will look for companies capable of meeting scaling demands, once they have settled on marketable models. Investment firm Morgan Stanley has been watching the EV industry, seeking out innovative new design and production companies that are positioning themselves for gains as the market matures. The firms automotive analyst, Adam Jonas, has selected two stocks that investors should seriously consider buying into, saying As we survey the EV/battery startup landscape, we are prioritizing highly differentiated technology and/or business models with a path to scale at a reasonable level of risk. Opening up the TipRanks database, weve pulled up the details on both of Jonas picks to see whether they could be a good fit for your portfolio. Fisker (FSR) First up, Fisker, is based in Southern California, the epicenter of so much of our ground-breaking tech industries. Fiskers focus is on solid-state battery tech, a growing alternative to the lithium-ion batteries that most EVs depend on. While more expensive that the older lithium-based systems, solid state batteries are safer and offer higher energy densities. Fisker has been busy patenting its moves into solid-state batteries, a sound strategy to lock in its advances in this field. For EVs, solid-state batteries offer faster charging times, longer range per charge, and potentially lower battery weight all important factors in vehicle performance. Every car company needs a flagship model, and Fisker has the Ocean an EV SUV with a mid-range price ($37,499) and a long-range power system (up to 300 miles). The vehicle features stylish design and room mounted solar panels to supplement the charging system, and is scheduled to enter serial production for the markets in 2022. The stylish design reflects the sensibilities of the companys founder, Henrik Fisker, known for his work on the BMW Z8 and the Aston Martin DB9. Fisker entered the public markets through a SPAC merger agreement last fall. Since completing the SPAC transaction on October 29, shares in FSR are up 112%. Morgan Stanleys Jonas is impressed by this company, describing the value proposition of Fisker as design, time to market, clean sheet user experience and management expertise, and saying that the 4Q22 launch schedule for the Ocean is likely to be met. Fisker is specifically targeting the personal owned/passenger car business as opposed to commercial oriented end markets, where emotive design and user experience matter more. Additionally, the company wants to create an all-digital experience from the website to the app to the HMI in the car and continued customer engagement through its flexible lease product, Jonas added. In line with his upbeat outlook on the company (and the car), Jonas rates Fisker an Overweight (i.e. Buy), and sets a $27 price target suggesting an upside of 42% for the coming year. (To watch Jonas track record, click here) Turning to the TipRanks data, weve found that Wall Streets analysts hold a range of views on Fisker. The stock has a Moderate Buy analyst consensus rating, based on 7 reviews, including 4 Buys, 2 Holds, and 1 Sell. Shares are currently priced at $18.99, and the $21.20 average price target implies a one-year upside of ~12%. (See FSR stock analysis on TipRanks) QuantumScape (QS) Where Fisker is working on solid-state batteries in the context of vehicle production, QuantumScape is setting itself up as a leader in EV battery technology and a potential supplier of the next generation of battery and power systems for the EV market. QuantumScape designs and builds solid-state lithium-metal batteries, the highest energy density battery system currently available. The key advantages of the technology are in safety, lifespan, and charging times. Solid-state batteries are non-flammable; they last longer than lithium-ion batteries, with less capacity loss at the anode interface; and their composition allows faster charging, of 15 minutes or less to reach 80% capacity. QuantumScape is betting that these advantages will outweigh the technologys current higher cost, and create a new standard in EV power systems. The companys strongest tie to the EV production field is its connection with Volkswagen. The German auto giant put $100 million into QuantumScape in 2018, and an additional $200 million in 2020. The two companies are using their partnership to prepare for mass-scale development and production of solid-state batteries. Like Fisker, QuantumScape went public through a SPAC agreement late last year. The agreement, which closed on November 27, put the QS ticker in the public markets where it promptly surged above $130 per share. While the stock has since slipped, it remains up 47% from its NYSE opening. For Morgan Stanleys Jonas, involvement in QS stock comes with high risk, but also high potential reward. In fact, the analyst calls it, "The Biotech of Battery Development." "We believe their solid state technology addresses a very big impediment in battery science (energy density) that, if successful, can create extremely high value to a wide range of customers in the auto industry and beyond. The risks of moving from a single layer cell to a production car are high, but we think these are balanced by the commercial potential and the role of Volkswagen to help underwrite the early manufacturing ramp," Jonas explained. Noting that QS is a stock for the long haul, Jonas rates the shares an Overweight (i.e. Buy), and his $70 price target indicates confidence in an upside of 28% for one-year time horizon. Granted, not everyone is as enthusiastic about QS as Morgan Stanly. QS's Hold consensus rating is based on an even split between Buy, Hold, and Sell reviews. The shares are priced at $54.64 and their recent appreciation has pushed them well above the $46.67 average price target. (See QS stock analysis on TipRanks) To find good ideas for EV stocks trading at attractive valuations, visit TipRanks Best Stocks to Buy, a newly launched tool that unites all of TipRanks equity insights. Disclaimer: The opinions expressed in this article are solely those of the featured analyst. The content is intended to be used for informational purposes only. It is very important to do your own analysis before making any investment.

Read more here:

FINAL DEADLINE: FIRST FILING AND TOP RANKED LAW FIRM, Encourages Sona Nanotech Inc. Investors with Large Losses to Secure Counsel Before Important...

Should We Be Delighted With Taiwan Advanced Nanotech Inc.’s (GTSM:6797) ROE Of 24%? – Simply Wall St

While some investors are already well versed in financial metrics (hat tip), this article is for those who would like to learn about Return On Equity (ROE) and why it is important. We'll use ROE to examine Taiwan Advanced Nanotech Inc. (GTSM:6797), by way of a worked example.

Return on Equity or ROE is a test of how effectively a company is growing its value and managing investors money. In simpler terms, it measures the profitability of a company in relation to shareholder's equity.

View our latest analysis for Taiwan Advanced Nanotech

Return on equity can be calculated by using the formula:

Return on Equity = Net Profit (from continuing operations) Shareholders' Equity

So, based on the above formula, the ROE for Taiwan Advanced Nanotech is:

24% = NT$56m NT$229m (Based on the trailing twelve months to June 2020).

The 'return' is the income the business earned over the last year. Another way to think of that is that for every NT$1 worth of equity, the company was able to earn NT$0.24 in profit.

Arguably the easiest way to assess company's ROE is to compare it with the average in its industry. The limitation of this approach is that some companies are quite different from others, even within the same industry classification. Pleasingly, Taiwan Advanced Nanotech has a superior ROE than the average (11%) in the Medical Equipment industry.

That's clearly a positive. With that said, a high ROE doesn't always indicate high profitability. A higher proportion of debt in a company's capital structure may also result in a high ROE, where the high debt levels could be a huge risk .

Virtually all companies need money to invest in the business, to grow profits. The cash for investment can come from prior year profits (retained earnings), issuing new shares, or borrowing. In the case of the first and second options, the ROE will reflect this use of cash, for growth. In the latter case, the debt required for growth will boost returns, but will not impact the shareholders' equity. That will make the ROE look better than if no debt was used.

While Taiwan Advanced Nanotech does have some debt, with a debt to equity ratio of just 0.31, we wouldn't say debt is excessive. The combination of modest debt and a very impressive ROE does suggest that the business is high quality. Judicious use of debt to improve returns can certainly be a good thing, although it does elevate risk slightly and reduce future optionality.

Return on equity is a useful indicator of the ability of a business to generate profits and return them to shareholders. Companies that can achieve high returns on equity without too much debt are generally of good quality. If two companies have the same ROE, then I would generally prefer the one with less debt.

But when a business is high quality, the market often bids it up to a price that reflects this. Profit growth rates, versus the expectations reflected in the price of the stock, are a particularly important to consider. You can see how the company has grow in the past by looking at this FREE detailed graph of past earnings, revenue and cash flow.

Of course Taiwan Advanced Nanotech may not be the best stock to buy. So you may wish to see this free collection of other companies that have high ROE and low debt.

PromotedWhen trading Taiwan Advanced Nanotech or any other investment, use the platform considered by many to be the Professional's Gateway to the Worlds Market, Interactive Brokers. You get the lowest-cost* trading on stocks, options, futures, forex, bonds and funds worldwide from a single integrated account.

This article by Simply Wall St is general in nature. It does not constitute a recommendation to buy or sell any stock, and does not take account of your objectives, or your financial situation. We aim to bring you long-term focused analysis driven by fundamental data. Note that our analysis may not factor in the latest price-sensitive company announcements or qualitative material. Simply Wall St has no position in any stocks mentioned. *Interactive Brokers Rated Lowest Cost Broker by StockBrokers.com Annual Online Review 2020

Have feedback on this article? Concerned about the content? Get in touch with us directly. Alternatively, email editorial-team (at) simplywallst.com.

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Should We Be Delighted With Taiwan Advanced Nanotech Inc.'s (GTSM:6797) ROE Of 24%? - Simply Wall St

Sona Nanotech, Inc. Investors: Last Days to Participate Actively in the Class Action Lawsuit; Portnoy Law Firm – Yahoo Finance

TipRanks

We are indeed living in interesting times and in many ways, thats a good thing. Take the automotive industry, for example. Technology is changing a rapid pace, and when it settles, it will dramatically change the way we drive. In 2030, our concept of car will likely be unrecognizable to drivers from 1980. The biggest changes are coming from power systems and artificial intelligence. AI will bring autonomous tech to our cars, making self-driving vehicles a reality. But the power systems changes will hit us first. In fact, electric-drive vehicles are already on our roads, and electric vehicle (EV) companies are proliferating rapidly. For the moment, there are several roads to potential success in the EV market. Companies are working to position themselves as leaders in battery tech, or electric power trains, or to maximize their range and performance per charge. Its a fact-paced industry environment, offering both opportunity and excitement for investors. Smart investors will look for companies capable of meeting scaling demands, once they have settled on marketable models. Investment firm Morgan Stanley has been watching the EV industry, seeking out innovative new design and production companies that are positioning themselves for gains as the market matures. The firms automotive analyst, Adam Jonas, has selected two stocks that investors should seriously consider buying into, saying As we survey the EV/battery startup landscape, we are prioritizing highly differentiated technology and/or business models with a path to scale at a reasonable level of risk. Opening up the TipRanks database, weve pulled up the details on both of Jonas picks to see whether they could be a good fit for your portfolio. Fisker (FSR) First up, Fisker, is based in Southern California, the epicenter of so much of our ground-breaking tech industries. Fiskers focus is on solid-state battery tech, a growing alternative to the lithium-ion batteries that most EVs depend on. While more expensive that the older lithium-based systems, solid state batteries are safer and offer higher energy densities. Fisker has been busy patenting its moves into solid-state batteries, a sound strategy to lock in its advances in this field. For EVs, solid-state batteries offer faster charging times, longer range per charge, and potentially lower battery weight all important factors in vehicle performance. Every car company needs a flagship model, and Fisker has the Ocean an EV SUV with a mid-range price ($37,499) and a long-range power system (up to 300 miles). The vehicle features stylish design and room mounted solar panels to supplement the charging system, and is scheduled to enter serial production for the markets in 2022. The stylish design reflects the sensibilities of the companys founder, Henrik Fisker, known for his work on the BMW Z8 and the Aston Martin DB9. Fisker entered the public markets through a SPAC merger agreement last fall. Since completing the SPAC transaction on October 29, shares in FSR are up 112%. Morgan Stanleys Jonas is impressed by this company, describing the value proposition of Fisker as design, time to market, clean sheet user experience and management expertise, and saying that the 4Q22 launch schedule for the Ocean is likely to be met. Fisker is specifically targeting the personal owned/passenger car business as opposed to commercial oriented end markets, where emotive design and user experience matter more. Additionally, the company wants to create an all-digital experience from the website to the app to the HMI in the car and continued customer engagement through its flexible lease product, Jonas added. In line with his upbeat outlook on the company (and the car), Jonas rates Fisker an Overweight (i.e. Buy), and sets a $27 price target suggesting an upside of 42% for the coming year. (To watch Jonas track record, click here) Turning to the TipRanks data, weve found that Wall Streets analysts hold a range of views on Fisker. The stock has a Moderate Buy analyst consensus rating, based on 7 reviews, including 4 Buys, 2 Holds, and 1 Sell. Shares are currently priced at $18.99, and the $21.20 average price target implies a one-year upside of ~12%. (See FSR stock analysis on TipRanks) QuantumScape (QS) Where Fisker is working on solid-state batteries in the context of vehicle production, QuantumScape is setting itself up as a leader in EV battery technology and a potential supplier of the next generation of battery and power systems for the EV market. QuantumScape designs and builds solid-state lithium-metal batteries, the highest energy density battery system currently available. The key advantages of the technology are in safety, lifespan, and charging times. Solid-state batteries are non-flammable; they last longer than lithium-ion batteries, with less capacity loss at the anode interface; and their composition allows faster charging, of 15 minutes or less to reach 80% capacity. QuantumScape is betting that these advantages will outweigh the technologys current higher cost, and create a new standard in EV power systems. The companys strongest tie to the EV production field is its connection with Volkswagen. The German auto giant put $100 million into QuantumScape in 2018, and an additional $200 million in 2020. The two companies are using their partnership to prepare for mass-scale development and production of solid-state batteries. Like Fisker, QuantumScape went public through a SPAC agreement late last year. The agreement, which closed on November 27, put the QS ticker in the public markets where it promptly surged above $130 per share. While the stock has since slipped, it remains up 47% from its NYSE opening. For Morgan Stanleys Jonas, involvement in QS stock comes with high risk, but also high potential reward. In fact, the analyst calls it, "The Biotech of Battery Development." "We believe their solid state technology addresses a very big impediment in battery science (energy density) that, if successful, can create extremely high value to a wide range of customers in the auto industry and beyond. The risks of moving from a single layer cell to a production car are high, but we think these are balanced by the commercial potential and the role of Volkswagen to help underwrite the early manufacturing ramp," Jonas explained. Noting that QS is a stock for the long haul, Jonas rates the shares an Overweight (i.e. Buy), and his $70 price target indicates confidence in an upside of 28% for one-year time horizon. Granted, not everyone is as enthusiastic about QS as Morgan Stanly. QS's Hold consensus rating is based on an even split between Buy, Hold, and Sell reviews. The shares are priced at $54.64 and their recent appreciation has pushed them well above the $46.67 average price target. (See QS stock analysis on TipRanks) To find good ideas for EV stocks trading at attractive valuations, visit TipRanks Best Stocks to Buy, a newly launched tool that unites all of TipRanks equity insights. Disclaimer: The opinions expressed in this article are solely those of the featured analyst. The content is intended to be used for informational purposes only. It is very important to do your own analysis before making any investment.

Go here to see the original:

Sona Nanotech, Inc. Investors: Last Days to Participate Actively in the Class Action Lawsuit; Portnoy Law Firm - Yahoo Finance

AREV Appoints Dr. Roscoe Moore to Join the Advisory Board – BioSpace

VANCOUVER, British Columbia, Feb. 09, 2021 (GLOBE NEWSWIRE) -- AREV NANOTEC BRANDS INC. (CSE: AREV) (OTC: AREVF) (AREV Brands) is pleased to announce the appointment of Dr. Roscoe Moore DVM, MPH, PhD, Former Assistant United States Surgeon General to the Scientific Advisory Board for AREV Nanotec Brands Inc, to provide strategic planning for AREV drug discovery planning, as a Senior Scientific Advisor.

Dr. Moore is a Board member of the Board of Advisors and the Board of Directors of the Global Virus Network at the Institute of Human Virology (IHV), University of Maryland Medical Center, According to theNational Science Foundation, UMBs budget for research and development in 2019 was $1.1 billion, ranking it 14th overall in the nation and 8th among all public institutions.

The IHV is the first research institute in the U.S. to link basic science, population studies and clinical trials in an effort to develop new vaccines and treatments. The IHV currently retains more than 300 employees include more than 80 faculty whose research efforts are focused on the area of chronic human viral infection and disease, and contributing to research on pandemic pathogens, ranging from COVID-19 to HIV.

Dr. Roscoe M. Moore Jr. served with the United States Department of Health and Human Services (HHS) and was responsible for the last twelve years of his career for global development support within the Office of the Secretary, HHS, with primary emphasis on implementing innovations in essential health care commodity procurement programs resource challenged countries. Dr. Moore was a career officer within the Commissioned Corps of the United States Public Health Service entering with the U.S. National Institutes of Health and rising to the rank of Assistant United States Surgeon General within the Immediate Office of the Secretary, HHS. Dr. Moore served as an Epidemic Intelligence Service Officer with the U.S. Centers for Disease Control and Prevention (CDC).

He was with the Center for Veterinary Medicine, U.S. Food and Drug Administration, before becoming Senior Epidemiologist within the National Institute for Occupational Safety and Health, CDC. Dr. Moore has conducted clinical research on infectious diseases, has evaluated the safety and effectiveness of medical devices, and has conducted relevant epidemiological research on the utilization experience and human health effects of medical devices and radiation. Dr. Moore served on the Fogarty International Center Advisory Board of Directors, NIH from 2009 to 2013. He served on the Alumni Board of Directors, School of Public Health, University of Michigan from 1987 to 1993. Dr. Moore served on the Deans Alumni Council, Bloomberg School of Public Health, at Johns Hopkins University from 1998 to 2002. He has also served as an Affiliate Associate Professor of Environmental Health for the University of Washington, Seattle from 1994 to 2003 and as an Adjunct Professor of Epidemiology, for the Medical University of Southern Africa, Pretoria, South Africa from 1999 to 2002. He served on the Board of Directors for the Africa Center for Health and Human Security, at George Washington University from 2006 to 2009.

AREV Nanotechs CEO, Mike Withrow commented Were very excited to welcome Dr. Moore to the AREV Nanotec Scientific Advisory Board. Dr Moores introduction to AREV Nanotech represents the emerging discovery opportunities beingpresented to the company now, as we pursue a range of pre-clinical investigations intended to identify antiviral phytomedicinal chemistries. This exciting focus is coming to also focusing on our emerging human and veterinary nutrition initiatives to improve global public health. Our intent to become a global leader in contributing to innovative therapeutic sustainable interventions that will be transformative to medicine and healthcare including our initial antiviral discovery program, AREVs human and veterinary nutrition product development and our competitive extraction science platform innovations, all of which are presenting very attractive opportunities to our investors and collaborators.

Dr. Moore commented, AREV Nanotech is developing a range of integrated extraction technologies that will help mature phytomedicinal discovery and advance promising therapies from bench to bedside. The necessity of advancing new innovations in discovery and subsequent therapeutics to address challenges in global public health. The current co-intersection of global pandemics emphasizes the value of companies like AREV which are focusing on the innovations to expand our current pharmacopeia to cultivate subsequent generations of phytomedicinal discovery."

The company has issued 250,000 stock options to Directors, Officers and Consultants of the Company at a price of $0.31 for a period of 5 years from the issued date. These options will vest immediately.

For further information, contact Mike Withrow, mike@AREVBrands.com 778-929-6536. For more information visitarevnanotec.com

On behalf of the Board,

Mike WithrowCEO & Director

About AREV NanoTec Inc. AREV NanoTec Brands Inc. (AREV) is an early stage publicly traded life science development enterprise focused on phytomedicinal extraction of novel therapeutic approaches to infectious diseases and subsequent comorbidities via its proprietary extraction systems to identify promising small molecules that present novel mechanisms of action in human and veterinary science.

AREVs model is to toll process extraction of targeted essential and functional oils and license its formulations to Licensed Producers in Canada.The company utilizes toll processors in foreign countries to encapsulate and package its formulations that can be sold in traditional distribution channels and online.

NEITHER THE CANADIAN SECURITIES EXCHANGE NOR ITS REGULATIONS SERVICES PROVIDER HAVE REVIEWED OR ACCEPT RESPONSIBILITY FOR THE ADEQUACY OR ACCURACY OF THIS RELEASE.

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AREV Appoints Dr. Roscoe Moore to Join the Advisory Board - BioSpace

Comprehensive Report on Nanotechnology Enabled Coatings for Aircraft Market 2021 | Trends, Growth Demand, Opportunities & Forecast To 2027…

Nanotechnology Enabled Coatings for Aircraft Market research report is the new statistical data source added by A2Z Market Research.

Nanotechnology Enabled Coatings for Aircraft Market is growing at a High CAGR during the forecast period 2021-2027. The increasing interest of the individuals in this industry is that the major reason for the expansion of this market.

Nanotechnology Enabled Coatings for Aircraft Market research is an intelligence report with meticulous efforts undertaken to study the right and valuable information. The data which has been looked upon is done considering both, the existing top players and the upcoming competitors. Business strategies of the key players and the new entering market industries are studied in detail. Well explained SWOT analysis, revenue share and contact information are shared in this report analysis.

Get the PDF Sample Copy (Including FULL TOC, Graphs and Tables) of this report @:

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Note In order to provide more accurate market forecast, all our reports will be updated before delivery by considering the impact of COVID-19.

Top Key Players Profiled in this report are:

AnCatt, Applied Thin Films, FlightShield, Glonatech, Triple, CHOOSE NanoTech, General Nano, HR ToughGuard, Surfactis Technologies, Tesla NanoCoatings.

The key questions answered in this report:

Various factors are responsible for the markets growth trajectory, which are studied at length in the report. In addition, the report lists down the restraints that are posing threat to the global Nanotechnology Enabled Coatings for Aircraft market. It also gauges the bargaining power of suppliers and buyers, threat from new entrants and product substitute, and the degree of competition prevailing in the market. The influence of the latest government guidelines is also analyzed in detail in the report. It studies the Nanotechnology Enabled Coatings for Aircraft markets trajectory between forecast periods.

Global Nanotechnology Enabled Coatings for Aircraft Market Segmentation:

Market Segmentation: By Type

Anti-corrosion, abrasion, and wear-resistant aircraft nanocoatingThermal barrier and flame retardant aircraft nanocoatingAnti-icing aircraft nanocoating

Market Segmentation: By Application

Commercial aircraftMilitary aircraft

Get up to 30% Discount on this Premium Report @:

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Regions Covered in the Global Nanotechnology Enabled Coatings for Aircraft Market Report 2021: The Middle East and Africa (GCC Countries and Egypt) North America (the United States, Mexico, and Canada) South America (Brazil etc.) Europe (Turkey, Germany, Russia UK, Italy, France, etc.) Asia-Pacific (Vietnam, China, Malaysia, Japan, Philippines, Korea, Thailand, India, Indonesia, and Australia)

The cost analysis of the Global Nanotechnology Enabled Coatings for Aircraft Market has been performed while keeping in view manufacturing expenses, labor cost, and raw materials and their market concentration rate, suppliers, and price trend. Other factors such as Supply chain, downstream buyers, and sourcing strategy have been assessed to provide a complete and in-depth view of the market. Buyers of the report will also be exposed to a study on market positioning with factors such as target client, brand strategy, and price strategy taken into consideration.

The report provides insights on the following pointers:

Market Penetration: Comprehensive information on the product portfolios of the top players in the Nanotechnology Enabled Coatings for Aircraft market.

Product Development/Innovation: Detailed insights on the upcoming technologies, R&D activities, and product launches in the market.

Competitive Assessment: In-depth assessment of the market strategies, geographic and business segments of the leading players in the market.

Market Development: Comprehensive information about emerging markets. This report analyzes the market for various segments across geographies.

Market Diversification: Exhaustive information about new products, untapped geographies, recent developments, and investments in the Nanotechnology Enabled Coatings for Aircraft market.

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Global Nanotechnology Enabled Coatings for Aircraft Market Research Report 2021 2027

Chapter 1 Nanotechnology Enabled Coatings for Aircraft Market Overview

Chapter 2 Global Economic Impact on Industry

Chapter 3 Global Market Competition by Manufacturers

Chapter 4 Global Production, Revenue (Value) by Region

Chapter 5 Global Supply (Production), Consumption, Export, Import by Regions

Chapter 6 Global Production, Revenue (Value), Price Trend by Type

Chapter 7 Global Market Analysis by Application

Chapter 8 Manufacturing Cost Analysis

Chapter 9 Industrial Chain, Sourcing Strategy and Downstream Buyers

Chapter 10 Marketing Strategy Analysis, Distributors/Traders

Chapter 11 Market Effect Factors Analysis

Chapter 12 Global Nanotechnology Enabled Coatings for Aircraft Market Forecast

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Conductive Inks Market to Witness Stunning Growth during 2021-2026 | Keyplayers : DuPont., Sun Chemical Corp, PPG Industries, Henkel AG, and Applied…

(Feb 2021) The latest report published by Polaris Market Research, titled Global Conductive Inks Market by Company, Region, Type and Application, Forecast for 2026provides key information about the current status and prospects of the market. The report focuses on market size, share, growth, emerging trends and market area analysis. The research also includes a comprehensive analysis of various market factors, including market drivers, restrictions, trends, risks, and opportunities that are common in the market.

The report provides an in-depth analysis of the global Conductive Inks market, which can help market participants design strategies and improve the profitability of their businesses. The study also outlines the major companies that exist in the market and their market shares, growth rates and product launches. The report covers the rapidly changing market scenario and covers the initial and future assessment of the impact

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The report produced by Polaris Market Research is widely known for its accuracy, because it is composed of precise charts, tables and graphs that clearly depict the development of past products and their market performance and predict future trends. It uses statistical surveys for SWOT analysis, PESTLE analysis, predictive analysis and real-time analysis.

Manufacturers covered in this report are:

DuPont., Sun Chemical Corp, PPG Industries, Henkel AG, and Applied Nanotech Holdings, Inc.

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In order to infer the market size, the report considered various aspects on the basis of secondary research. In addition, data points such as product segmentation and market segmentation are also divided by end use. It also combines the qualitative opinions of the main interviewees to arrive at an appropriate market estimate. The forecast provided in the report assesses the total revenue generated by the Conductive Inks market and the expected revenue contribution.

When formulating market forecasts, the report will determine the size of the current market, which is the basis for predicting how the market will form in the near future. Market Insights triangulates data through different analysis based on supply side, demand side and other dynamics. The report not only provides CAGR forecasts, but also analyzes the market based on key parameters such as year-on-year (Y-o-Y) growth to understand the predictability of the market and identify the right opportunities.

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Conductive Inks Market to Witness Stunning Growth during 2021-2026 | Keyplayers : DuPont., Sun Chemical Corp, PPG Industries, Henkel AG, and Applied...

Mars Facts – Interesting Facts about Planet Mars

Mars is the fourth planet from the Sun and is the second smallest planet in the solar system. Named after the Roman god of war, Mars is also often described as the Red Planet due to its reddish appearance. Mars is a terrestrial planet with a thin atmosphere composed primarily of carbon dioxide.

Mars has two small moons, Phobos and Deimos. They were discovered in 1877 by astronomer Asaph Hall, who named them for the Latin terms fear and panic. These moons are thought to be captured asteroids and are among the smallest natural satellites in the solar system.

Mars has the largest volcano in the solar system Olympus Mons. It measures some 600 kilometres across and rises nearly 27 kilometres above the surrounding terrain. It is a shield volcano built by the continuous action of flowing lava over millions and millions of years that began some 3 billion years ago.

Olympus Mons is part of a complex of volcanoes that lie along a volcanic plateau called the Tharsis Bulge. This entire region lies over a hotspot, a place in the planets crust that allows magma from deep inside to flow out to the surface.

The Valles Marineris is an extensive canyon system on the Mars equator. It is 4,200 kilometres long and, in places, is 7 kilometres deep. On Earth, it would span the entire North American continent and beyond.

Mars has has a very primitive form of plate tectonics, and the action of two plates past each other began splitting the surface some 3.5 billion years ago. That set the stage for the formation of the Valles Marineris.

Sources: https://solarsystem.nasa.gov/planets/mars/overview/ , https://nssdc.gsfc.nasa.gov/planetary/factsheet/marsfact.html, https://astrogeology.usgs.gov/maps/mars-viking-hemisphere-point-perspectives First Published: June 2012Last Updated: May 2020Author: Chris Jones

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Mars Facts - Interesting Facts about Planet Mars

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Why Mars is having its busiest two weeks in 47 years – Livescience.com

It's a busy February for Mars, with three probes from three separate countries arriving at the Red Planet over the course of just nine days. But this Martian party didn't happen by coincidence it has to do with the mechanics of both Earth and Mars orbits.

The United Arab Emirates' first interplanetary mission, the Hope probe, achieved Mars orbit Tuesday (Feb. 9), as Live Science sister site Space.com reported. China's first interplanetary mission, Tianwen-1, is scheduled to enter its own Martian orbit Wednesday (Feb. 10). The Chinese probe includes both an orbiter and a lander with a rover onboard, which is expected to try to land on the surface in May. And on Feb. 18, NASA's first-of-its-kind descent vehicle will reach Mars and plunge directly through its atmosphere. If all goes according to plan, the vehicle will shed its outer shell and use rockets to stop its descent at the last moment. Then it will hover above the surface to lower the rhinoceros-sized, nuclear-powered, $2.7 billion Perseverance rover to the dirt via skycrane.

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All these robots showing up at almost the exact same time is no coincidence, said Jonathan McDowell, a Harvard University astrophysicist and spaceflight expert.

Mars and Earth are like "runners on a circular racetrack," he said. "And the really fast runner [Earth] regularly laps the runner just on the outside [Mars]. So sometimes they're right next to each other, and sometimes they're on opposite sides of the track." This Earth-Mars cycle, meaning Earth completely laps Mars, takes about two years to complete.

It would take an enormous rocket, tons of fuel and much more time to reach Mars from Earth while the planets are far away from each other, McDowell told Live Science. But launching while the planets are at their absolute closest when they are 38.6 million miles (62.1 million kilometers) apart on average isnt the most efficient way to get to Mars either.

There's an earlier point in the planets' two-year cycle where the journey takes less time and requires less fuel. At that point, which occurs once during the two-year cycle, Earth is a bit behind Mars but continues to move faster than its neighbor. This positioning allows the spacecraft to enter a so-called "Hohmann transfer orbit," named after German engineer Walter Hohmann, who worked out the underlying mathematics in 1925.

Related: 5 Mars myths and misconceptions

Here's how that works:

No rocket carries enough fuel to burn all the way between Earth and Mars, a distance that ranges between tens and hundreds of millions of miles.

That means any interplanetary adventure begins with a brief, intense period of acceleration, followed by a long stretch of coasting. The job of the rocket engines during that initial period of acceleration is to put the spacecraft into an orbit around the sun that will intersect with Mars as soon as possible. The most efficient path between the planets is therefore the solar orbit intersecting with Mars that can be reached with the least expenditure of fuel, and that orbit becomes available once every two years.

But space agencies don't have to nail that day exactly. As long as they launch during a window of a couple weeks around the date,they can place their spacecraft on Hohmann transfer orbits. Tarry longer than a couple weeks, however, and the trip starts getting much more difficult very quickly.

The Hope orbiter launched July 19, 2020, Tianwen-1 on July 23 and Perseverance on July 30. The gaps between the spacecrafts' arrivals don't exactly line up with their launch dates due to minor differences in their rocket technology, trajectories through space and destinations, McDowell said. (It takes a different angle of approach, for example, to plunge directly into the planet's atmosphere than it does to enter a high orbit as Hope has done.)

It's not the first time Martian orbital space has been this crowded, McDowell pointed out. The Soviet Union launched four spacecraft to Mars in 1973, though one failed to attain orbit and none of the other three worked as intended upon arrival. Two Soviet spacecraft and one American spacecraft launched to Mars in 1971, and all had at least partially successful missions. (Both nations planned additional probes that year, but the American Mariner 8 probe failed during launch and the Soviet Kosmos 419 never escaped low-Earth orbit.)

Related: Here's every spaceship that's ever carried an astronaut into orbit

What's different this year, McDowell said, is the sheer diversity of spacecraft reaching Mars, and the fact that several additional probes are already active around the planet. NASA has three orbiters active in Martian orbit, the European Space Agency (ESA) has one of its own and one orbiter that's a joint project with the Russian Roscosmos, and the Indian Space Research Organization has an active orbiter as well. NASA's Curiosity rover and InSight lander are also still active on the Martian surface.

Despite that relatively crowded situation, McDowell said he doubts any of the probes will even come within tens of thousands of miles of each other, even if none of the countries had checked their trajectories with each other in advance.

"Space is big," he said.

Originally published on Live Science.

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Why Mars is having its busiest two weeks in 47 years - Livescience.com

Where Should Future Astronauts Land on Mars? Follow the Water NASA’s Mars Exploration Program – NASA Mars Exploration

A new NASA paper provides the most detailed map to date of near-surface water ice on the Red Planet.

So you want to build a Mars base. Where to start? Like any human settlement, it would be best located near accessible water. Not only will water be crucial for life-support supplies, it will be used for everything from agriculture to producing the rocket propellant astronauts will need to return to Earth.

Schlepping all that water to Mars would be costly and risky. Thats why NASA has engaged scientists and engineers since 2015 to identify deposits of Martian water ice that could be within reach of astronauts on the planets surface. But, of course, water has huge scientific value, too: If present-day microbial life can be found on Mars, it would likely be nearby these water sources as well.

A new study appearing in Nature Astronomy includes a comprehensive map detailing where water ice is most and least likely to be found in the planets northern hemisphere. Combining 20 years of data from NASAs Mars Odyssey, Mars Reconnaissance Orbiter, and the now-inactive Mars Global Surveyor, the paper is the work of a project called Subsurface Water Ice Mapping, or SWIM. The SWIM effort is led by the Planetary Science Institute in Tucson, Arizona, and managed by NASAs Jet Propulsion Laboratory in Southern California.

The next frontier for Mars is for human explorers to get below the surface and look for signs of microbial life, said Richard Davis, who leads NASAs efforts to find Martian resources in preparation for sending humans to the Red Planet. We realize we need to make new maps of subsurface ice to improve our knowledge of where that ice is for both scientific discovery and having local resources astronauts can rely on.

In the near future, NASA plans to hold a workshop for multidisciplinary experts to assess potential human-landing sites on Mars based on this research and other science and engineering criteria. This mapping project could also inform surveys by future orbiters NASA hopes to send to the Red Planet.

NASA recently announced that, along with three international space agencies, the signing of a statement of intent to explore a possible International Mars Ice Mapper mission concept. The statement brings the agencies together to establish a joint concept team to assess mission potential as well as partnership opportunities between NASA, the Agenzia Spaziale Italiana (the Italian Space Agency), the Canadian Space Agency, and the Japan Aerospace Exploration Agency.

Location, Location, Location

Ask Mars scientists and engineers where the most accessible subsurface ice is, and most will point to the area below Mars polar region in the northern hemisphere. On Earth, this region is where you find Canada and Europe; on Mars, it includes the plains of Arcadia Planitia and glacier-filled valleys in Deuteronilus Mensae.

Such regions represent a literal middle ground between where to find the most water ice (the poles) and where to find the most sunlight and warmth (the equator). The northern midlatitudes also offer favorable elevations for landing. The lower the elevation, the more opportunity a spacecraft has to slow down using friction from the Martian atmosphere during its descent to the surface. Thats especially important for heavy human-class landers, since Mars atmosphere is just 1% as dense as Earths and thus provides less resistance for incoming spacecraft.

Ultimately, NASA tasked the SWIM project with figuring out how close to the equator you can go to find subsurface ice, said Sydney Do, the Mars Water Mapping Project lead at JPL. Imagine weve drawn a squiggly line across Mars representing that ice boundary. This data allows us to draw that line with a finer pen instead of a thick marker and to focus on parts of that line that are closest to the equator.

But knowing whether a surface is hiding ice isnt easy. None of the instrument datasets used in the study were designed to measure ice directly, said the Planetary Science Institutes Gareth Morgan, the SWIM-project co-lead and the papers lead author. Instead, each orbiter instrument detects different physical properties high concentrations of hydrogen, high radar-wave speed, and the rate at which temperature changes in a surface that can suggest the presence of ice.

Despite having 20 years of data and a fantastic range of instruments, its hard to combine these datasets, because theyre all so different, Morgan said. Thats why we assessed the consistency of an ice signal, showing areas where multiple datasets indicate ice is present. If all five datasets point to ice bingo.

If, say, only two of them did, the team would try to suss out how consistent the signals were and what other materials could be creating them. While the different datasets werent always a perfect fit, they often complemented one another. For example, current radars peer deep underground but dont see the top 30 to 50 feet (10 to 15 meters) below the surface; a neutron spectrometer aboard one orbiter measured hydrogen in the uppermost soil layer but not below. High-resolution photos revealed ice tossed onto the surface after recent meteorite impacts, providing direct evidence to complement radar and other remote-sensing indicators of water ice.

Next Steps

While Mars experts pore over these new maps of subsurface ice, NASA is already thinking about what the next steps would be. For one, blind spots in currently available data can be resolved by sending a new radar mission to Mars that could home in on the areas of greatest interest to human-mission planners: water ice in the top layers of the subsurface.

A future radar-focused mission targeting the near surface could also tell scientists more about the mix of materials found in the layer of rock, dust, and other material found on top of ice. Different materials will require specialized tools and approaches for digging, drilling, and accessing water-ice deposits, particularly in the extreme Martian environment.

Mapping efforts in the 2020s could help make human missions to Mars possible as early as the 2030s. But before that, therell be a robust debate about the location of humanitys first outpost on Mars: a place where astronauts will have the local water-ice resources needed to sustain them while also being able to make high-value discoveries about the evolution of rocky planets, habitability, and the potential for life on worlds beyond Earth.

News Media ContactsAndrew GoodJet Propulsion Laboratory, Pasadena, Calif.818-393-2433andrew.c.good@jpl.nasa.gov

Alana Johnson / Grey HautaluomaNASA Headquarters, Washington202-672-4780 / 202-358-0668alana.r.johnson@nasa.gov / grey.hautaluoma-1@nasa.gov

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Where Should Future Astronauts Land on Mars? Follow the Water NASA's Mars Exploration Program - NASA Mars Exploration

Transient HCl in the atmosphere of Mars – Science Advances

Abstract

A major quest in Mars exploration has been the hunt for atmospheric gases, potentially unveiling ongoing activity of geophysical or biological origin. Here, we report the first detection of a halogen gas, HCl, which could, in theory, originate from contemporary volcanic degassing or chlorine released from gas-solid reactions. Our detections made at ~3.2 to 3.8 m with the Atmospheric Chemistry Suite and confirmed with Nadir and Occultation for Mars Discovery instruments onboard the ExoMars Trace Gas Orbiter, reveal widely distributed HCl in the 1- to 4-ppbv range, 20 times greater than previously reported upper limits. HCl increased during the 2018 global dust storm and declined soon after its end, pointing to the exchange between the dust and the atmosphere. Understanding the origin and variability of HCl shall constitute a major advance in our appraisal of martian geo- and photochemistry.

Chlorine is present in the atmospheres of Earth and Venus and plays a critical role in their photochemical cycles. In Earths troposphere, hydrogen chloride (HCl) is mainly sourced from sea salt aerosols, and its abundance partly controls the oxidizing potential of the atmosphere by interacting with ozone and hydroxyl radicals (OH) (1). In the stratosphere, relatively inert HCl is the main reservoir species, releasing chlorine radicals in heterogeneous processes that subsequently participate in ozone layer chemistry and seasonal polar ozone depletion. On Venus, HCl is also the dominant reservoir of chlorine, and its destruction via photolysis produces reactive chlorine species that are critical to the stability of its CO2 atmosphere (2). HCl has never been observed in the atmosphere of Mars but has been suggested and sought as an indicator of active magmatic processes (3). Stringent upper limits of 0.2 to 0.3 parts per billion volume (ppbv) were established (4, 5).

The primary science goal of the European Space Agency (ESA)Roscosmos ExoMars Trace Gas Orbiter (TGO) mission is to make highly sensitive measurements of trace atmospheric species, including volcanic gases (6). TGO carries two dedicated spectrometers, the Atmospheric Chemistry Suite (ACS) (7) and the Nadir and Occultation for Mars Discovery (NOMAD) suite (8). From the start of the mission in April 2018, the TGO instruments measured multiple known atmospheric gases and their isotopologues (915).

Here, we discuss the first positive detection of a previously undetected gas-phase molecule in the atmosphere of Mars by TGO, hydrogen chloride (HCl). Figure 1 shows a sequence of spectra that highlight the HCl absorption features detected by ACS. They were measured on 4 January 2019 at 73S latitude [heliocentric solar longitude (LS) = 318, late northern winter or southern summer on Mars]. As the instruments line of sight (LOS) moves deeper into the atmosphere during a solar occultation (SO) (7), we can retrieve the vertical profile of the HCl mixing ratio (see Materials and Methods). The spectra are zoomed on the spectral ranges around three distinct features in the R branch of the HCl 10 transition band. The depth of absorption due to HCl reaches 3 to 4%, while the signal-to-noise ratio per pixel of the instrument, although dependent on the dust content in the atmosphere, is generally over 3000 to 5000. Neighboring absorption lines in Fig. 1 are caused by water, semiheavy water (HDO), and the H37Cl isotopologue of HCl. In all, ACS detects 12 spectral features belonging to H35Cl and H37Cl in the P and R branches of its 1 fundamental rotational band.

Each panel shows spectra recorded as sequential tangent heights, indicating how the HCl features evolve with altitude. The occultation shown was recorded on LS = 318 at a latitude 73.5.

Figure S1 shows the wider spectral range covered by ACS and the contributions of different gases, and fig. S2 shows fits for HCl lines not shown in Fig. 1. The detection of HCl by ACS is corroborated by NOMAD measurements. HCl can be detected using several diffraction orders covering the 2600 to 3100 cm1 spectral range (see fig. S3). The vertical profiles of the HCl mixing ratio are presented in Fig. 2. We observe three families of altitude profiles. In the Northern Hemisphere, mixing ratios of 1 to 2 ppbv are observed mostly at altitudes in the range of 15 to 25 km, decreasing toward the surface (Fig. 2A). In the Southern Hemisphere, a series of observations were made prior to LS = 300, during which time we were unable to probe below 15 km, but observed 2 to 3 ppbv between 20 and 30 km (Fig. 2B). After LS = 300, we observed higher abundances, but HCl was entirely constrained below 15 km (Fig. 2C). The differences between Fig. 2 (B and C) reflect changes in the physical state of the atmosphere as the dust storm declines, which are also tracked by water vapor and aerosols. During this time, dust settled to the surface and lower atmosphere, followed by cooling and contraction, and a lowering of the hygropause.

Profiles are grouped as (A) Northern Hemisphere observations between LS = 210 and 330, (B) Southern Hemisphere observations between LS = 245 to 290, and (C) Southern Hemisphere observation between LS = 310 and 325. Retrievals on a 1-km grid are shown as solid lines, and retrievals at the tangent heights are shown at points with uncertainties derived from the retrievals matrix of partial derivatives. The mean of the ensemble is shown in purple with a shaded area showing the SD. The ensemble of retrievals is shown in fig. S4.

A latitudinal map of all HCl detections and upper limits is shown in Fig. 3A as a function of time, from LS = 163 in Mars Year 34 (MY34) (April 2018) to LS = 166 in MY35 (March 2020). For observations where HCl is not observed, a lower limit is given (see fig. S5), which is generally <0.2 ppbv and often ~0.1 ppbv. No firm detection was made between the beginning of the TGO science phase until the global dust storm (GDS) period. A few values have been retrieved with a 1-sigma confidence level, but they have the same magnitude (<1 ppbv) as the upper limits established in nearby occultations and those previously set by ground-based observations of 0.3 to 0.6 ppbv (4, 5). HCl is detected starting from LS = 230 and persists until around LS = 350. There are over 140 positive detections made by ACS and nearly 50 by NOMAD over the same time period.

All ACS MIR occultations are shown in gray, and those with the spectral range used for HCl, but not bearing strong HCl signatures, are shown as triangles, with the color indicating a lower limit of the HCl VMR. Observations with detected HCl lines are indicated with circles and colored by their maximum retrieved HCl mixing ratio at between 10 and 30 km. Additional retrievals using NOMAD SO are shown with diamonds. Science operations began on LS = 163 in MY34 and continued through LS = 166 in MY35 at the time of writing. The GDS commenced around 190 and was followed by a second storm around LS = 320, and the mean dust opacity (16) is shown in (A). (B) The corresponding lowest usable tangent height for ACS observations, limited by transmission levels below this point being only a few percent.

This time period, coinciding with seasonally enhanced dust, was punctuated by the onset of a GDS, beginning in the Southern Hemisphere around LS = 190, followed by a second, regional, storm at around LS = 320, with dust persisting through LS = 190 to 350 (16). The dust, lofted to heights of 30 to 50 km, is radiatively active and causes the atmosphere to heat and expand while intensifying Hadley cell circulation. Water vapor normally restricted to near the surface is elevated to create a hygropause near 80 km with mixing ratios around 150 ppmv, as observed by TGO (11, 12) and reproduced by modeling (17). Dust affects SO observations in such a way that the dust storm imposed limits on the lowest observable altitude of TGO instruments. Figure 3B shows the corresponding minimum altitude in the atmosphere that we can observe due to aerosol loading (see also fig. S6). Still, even during the peak of the GDS, polar latitudes remained relatively free from aerosols. During this period, we begin to see HCl frequently in the Northern and Southern Hemispheres, suggesting HCl was already present and spread by atmospheric circulation. During the decline of the storm (from LS ~ 240) and through the whole perihelion season, the map shows the densest, quasi-complete presence of HCl in both hemispheres, including a few detections at mid-latitudes, where observation conditions are not optimal. After the second regional dust storm of MY34, the detections become less frequent, and during MY35, we only occasionally see low levels of HCl in our spectra. At LS = 75, the HCl upper limit of ~0.1 ppbv that we derive from ACS is consistent with the upper limit of 0.3 ppbv (3-sigma) previously determined at the same season from the Herschel satellite (4).

The observations just described suggest that the source of HCl is aerosol chemistry occurring with the dust particles lofted into the atmosphere. However, this is not the only possible source of HCl, and the distributions observed by TGO may result from several possible interactions that may be interrelated. We must also emphasize that the geometry of the SO technique does not always allow us to observe the lowest few kilometers of the atmosphere that may also contain HCl, while previous searches for HCl observed the full atmospheric column and were sensitive to these layers.

An alternative explanation for the presence of HCl in the martian atmosphere is as a result of recent surface volcanism or subsurface magmatic activity. HCl is a minor gas emitted by terrestrial volcanism, and past martian volcanism has been suggested to be the source of contemporary surface chloride minerals (18). However, we note that outgassing of HCl related to magmatism (whether directly at the surface or at depth) should be accompanied by seismic activity and a suite of other sulfur-bearing and carbon-bearing molecules. Such molecules, SO2 in particular, have not been detected on Mars so far (19), and no correlation of HCl observations with Marsquakes measured by the InSight lander is apparent [noting that InSight measurements began at the end of February 2019 (LS = 340) and that seismicity on Mars is lower than projected (20)]. In addition, the fact that the HCl increase is detected almost simultaneously at very distant locations of both hemispheres is difficult to reconcile with local release at the surface.

In the terrestrial troposphere, the majority of the HCl is not volcanic but produced from reactions between acids and hydrated NaCl originating from sea-salt aerosols (21). While there are no marine aerosols currently produced on Mars, there is a notable coincidence between HCl detections made here and the particularly strong GDS of MY34. This suggests that physical or chemical processes in martian dust storms may trigger the release of reactive gas-phase chlorine from the material that constitutes the airborne dust. Chlorine is widespread at the surface (22), and in the martian dust, at levels reaching 1 % by weight (23). This chlorine may be present as halite (NaCl), a mineral observed in nakhlite meteorites that originated from Mars (24) and proposed to be the dominant form of chloride on the martian surface in certain areas observed from orbit (25). Alternatively, perchlorate (ClO4) has been observed on the martian surface at high and low latitudes (26, 27) and should be widely distributed (28). During a dust storm event, both of these forms of Cl may be lofted into the atmosphere, making chlorine readily available in the lower atmosphere at this time. Releasing gas-phase chlorine from chloride salts may involve hydration of the chlorine salts, which has been shown to be effective in martian conditions (29). This can be followed by oxidation reactions and the release of radicals. The latter mechanism remains speculative at martian conditions but would ultimately lead to the formation of HCl (30).

In detail, four different pathways can be considered: (i) As the GDSs, and that of 2018 in particular, are characterized by large H2O mixing ratios up to very high altitudes (11, 12, 31), unusually strong concentrations of oxidants such as OH and HO2 should be expected in the atmosphere. In this case, particularly efficient gas-surface oxidation processing of the dust aerosols during the GDS may release reactive chlorine, as is the case on Earth (1, 30). This scenario is supported by a strong correlation between the observed HCl and H2O profiles (see fig. S7). A simultaneous observation of elevated HCl, H2O, and aerosols, which are governed by the same advection pattern, does not constitute direct evidence of a cause-and-effect relation between them. However, the detection of a sudden appearance of HCl only in the presence of dust (furthermore during unfavorable viewing conditions caused by the dust-rich environment) provides strong indirect support for this hypothesis.

(ii) Chlorine would be more efficiently released from dust via acidic oxidation, analogous to terrestrial processes. The availability of necessary acids in the martian atmosphere remains unknown, but photochemical modeling studies (32, 33) have demonstrated that the presence of nitrates, identified on the martian surface (34) and a likely component of dust, should enable the production of acids, nitric acid (HNO3), and peroxynitric acid (HNO4). They oxidize dry chloride salts to make Cl2 gas, which would rapidly photolyze to generate chlorine radicals (35), which then react with HO2 (primarily) to form HCl.

(iii) Because of strong saltation processes, the GDS can mobilize dust grains that have not been previously exposed to UV light for long periods. Being lifted to high altitudes, chlorine-bearing molecules at the surface of airborne dust may break up under the effect of UV irradiation into gas-phase compounds, including chlorine. The potential to oxidize mineral chlorides by the action of UV radiation has been demonstrated in the laboratory (36), but more experimental work is required to determine the abundance of chloride radicals that could be released to the gas phase by such processes.

(iv) Chlorine could be released by the volatilization of chloride minerals by electrical discharges in the dust storm, as demonstrated in laboratory experiments under simulated martian atmosphere conditions (3739).

The decline in HCl, observed by ACS in MY35, is also indicative of an unexpected chemical sink for that species, which, in terms of the conventional gas-phase chemistry, is the stable reservoir of chlorine in the lower atmosphere of Mars (40). The transient nature of the observed HCl tells us that this does not constitute the whole picture and that we are missing an important chemical or physical loss process of chlorine. On Earth, laboratory studies have demonstrated the strong uptake coefficient of HCl on water ice surfaces at temperatures typical of those encountered on Mars (41, 42). Water ice clouds are detected in our occultations during the whole dusty period, overlaying the dust, and, later, at lower altitudes, where we see HCl (12, 43). In addition, surface frost is at a maximum at LS = 270 (northern winter), when our northern HCl values are smaller. Heterogeneous HCl loss on surface ice would also be compatible with the shape of the profiles shown in Fig. 2 (A and C), showing decreasing mixing ratios near the surface.

Although our data do not permit a definitive determination of the source of HCl at this time, the coincidence of the GDS leads us to propose a novel surface-atmosphere interaction made plausible by terrestrial chemistry and recent laboratory studies. General circulation modeling is needed to constrain rates of HCl production and destruction and to probe possible sources of surface venting. The apparent link to dust activity will be examined during future dust events. Regardless of the HCl origin, it appears unlikely that the processes responsible for its production and destruction would not affect the rest of Mars atmospheric chemistry. An impact on other gases is expected at altitudes above 30 km, where a greater fraction of chlorine is in the form of atomic Cl. The peak HCl concentrations on Mars ~1 to 4 ppbv are comparable to those in Earths upper stratosphere and mesosphere (44). On Mars, the destructive ozone cycle, including odd oxygen, well known in Earths stratosphere (45), would be ~20 times more efficient than assumed with previous upper limits on HCl. On the other hand, the transient nature of the HCl enhancement detected by ACS suggests the existence of a strong and unexpected loss process of that species, likely heterogeneous and efficient in the lower atmosphere or at the surface of Mars. Such a pathway may be photochemical and related to the advection pattern of other gases, such as H2O, or to the absorption by dust itself (46). Our discovery suggests that the martian photochemistry should be revised, considering reactions with atmospheric dust or surface outgassing.

The ACS instrument is a collection of three spectrometers operating in nadir and SO mode. The work presented here uses the ACS mid-infrared (ACS MIR) channel, which is a cross-dispersion echelle spectrometer. Solar light is dispersed by an echelle grating to measure the spectrum in the infrared range with high spectral resolving power (/ ~ 30,000). Overlapping diffraction orders are then separated by a steerable secondary diffraction grating, the position of which determines the instantaneous spectral range (7). In this study, we use secondary grating positions 11 and 12, which provide spectral ranges of 2678 to 2948 cm1 and 2917 to 3235 cm1, respectively, and divided into 16 to 20 diffraction orders. The diffraction orders related to the fundamental rotational band of HCl are shown in fig. S1, along with the contributions to transmission spectra by the absorption of CO2, H2O, HDO, and HCl. The partial overlap of the instantaneous spectral range in positions 11 and 12 permits measuring diffraction orders 173 to 175 in both positions. Figure S2 shows fits to HCl lines from both grating positions, in orders not presented in Fig. 1.

An ACS MIR detector image is a two-dimensional array of measured intensities. The x axis corresponds to wave number calibration, and the y axis corresponds to both the diffraction order and the tangent height of the instantaneous field of view (IFOV) (7). The appearance of a frame is several brightness stripes approximately 20 pixels wide, each one corresponding to a diffraction order in the mid-infrared (14). The IFOV covers 1 to 4 km, and each row provides a unique spectrum, separated by ~0.1 km.

Processing of the detector images was carried out at the Space Research Institute of the Russian Academy of Sciences (IKI RAS). A set of corrections is applied to each data frame that includes masking hot pixels, accounting for a subpixel drift in position caused by the instruments thermal state, and an orthorectification. A dark image (Idark) accounting for dark current and thermal drift is computed from the observations made when the sun is fully obscured. A solar reference image (Isun) is computed by stacking observations made at tangent heights from 80 to ~250 km. For the spectral range provided by secondary grating positions 11 and 12, 80 km is sufficiently high to be free of gaseous absorption. The transmission at each altitude z is computed from the observations I(z) as (I(z) Idark)/(Isun Idark). Additional details can be found in (1214, 47).

In ACS MIR, there is an effect, possibly caused by an optical component being damaged during launch, that results in the image of gaseous absorption lines to appear doubled. Rows for analysis are chosen by identifying the edge of the detector slit closest to the center of the solar disk, where this effect is minimized (a small shoulder is visible in spectra shown in fig. S2) (10, 13, 14). An instrument line shape can be modeled that accounts for this feature, and we have shown that it can be used to accurately retrieve trace gas abundances by validating results against those obtained from simultaneous observations made by the near-infrared (NIR) channel of ACS (9, 10, 12, 13). Wave number calibration is performed for each row in two steps: first, by comparing the solar reference spectra to that measured by the Atmospheric Chemistry Experiment Fourier Transform Spectrometer (ACE-FTS) (48), and then, by comparing strong gas absorption lines, when available (13). Lastly, spectra are normalized using an alpha hull method (49).

Spectral fitting was performed using the Jet Propulsion Laboratory Gas Fitting Software suite (GGG or GFIT) (5052). The atmosphere is modeled as homogeneous layers of 1-km thickness, and the optical path through each layer along the LOS is computed. For each fitting interval and for each spectrum, a forward model is computed using the instrument line shape described above and a Voigt line shape that depends on temperature and pressure and broadening parameters taken from the 2016 version of HITRAN line list (53). Vertical profiles of temperature and pressure were retrieved from CO2 absorption features in simultaneous observations made by ACS NIR (12). The line depths are related to a gas mixing ratio through the Beer-Lambert law, which depends on the line strength, taken from HITRAN 2016, the line shape, the temperature, and pressure of the atmosphere, and the optical path length. Vertical profiles of trace gas volume mixing ratios (VMRs) are estimated by inverting a matrix of LOS column abundances with a matrix of atmospheric layer contributions along the optical path. Uncertainties are computed from the Jacobian matrix of partial derivatives.

ACS results have been confirmed by two other analysis streams developed at the IKI and the Laboratoire Atmosphres, Milieux, Observations Spatiales (LATMOS) in support of the Mars Express Spectroscopy for Investigation of Characteristics of the Atmosphere of Mars instrument (31, 54). The IKI code uses a Levenberg-Marquardt iterative approach to find the best solution for the gaseous composition of a model atmosphere, followed by applying Tikhonov regularization of the profile. This code has been adapted and used with ACS MIR (9) and ACS NIR (12) data. The LATMOS code uses a Levenberg-Marquardt regression scheme applied to transmittance spectra to infer the LOS integrated quantities of gases (47). The VMR is obtained by rationing the simultaneous observations of the targeted species (HCl in that case) with that of CO2 calculated from fitting its 628 isotope Q branch in diffraction order 178. Derived gaseous vertical profiles are subsequently smoothed by convolving with a 1-km Gaussian kernel.

Detection limits have been estimated by measuring the noise of each spectrum and then performing spectral fitting with fixed quantities of HCl until modeled lines become prominent enough to cross a threshold value. The noise is measured by computing the difference between a spectrum and a smoothed spectrum. A smoothing window sufficiently wide to capture the variability of the signal caused by both random noise and larger systematic features is used, resulting in an SD of the noise that is consistent with that of the residuals of good spectral fits. A modest 2 SD threshold from a mean spectrum baseline value was used. The mean values, 1 and 2 SD thresholds, best-fit lines, and modeled spectra are shown in fig. S5 (A and B) for diffraction orders 174 and 175. The mean detection limit for these two orders, common to grating positions 11 and 12, is used to compute vertical profiles of detection limits, a selection of which are shown in fig. S5C. This method results in larger, more modest detection limits, appropriate for a gas that is now known to be present, than using the retrieval uncertainties. It is also more robust, as a best-fit line can occasionally suggest a negative gas value, which results in larger oscillation in a vertical profile of retrieval uncertainties. In total, 643 occultations have been analyzed in Fig. 3.

NOMAD is a set of spectrometers operating in the spectral ranges between 0.2 and 4.3 m consisting of three channels. HCl has been observed with the SO channel, which uses an echelle grating used in combination with an acousto-optic tunable filter (AOTF) that selects the diffraction orders to be recorded (8, 55). The diffraction order can be changed instantaneously by altering the frequency applied to the AOTF, and so, the SO channel is able to measure any five or six selected diffraction orders per second within the entire spectral range of the channel. The illuminated rows on the detector are split into four individual bins, and a spectrum is recorded for each bin in every diffraction order from the top of the atmosphere (~200 km) to near the surface. Wave number calibration uses gaseous absorption lines, and a correction is applied to account for pixel nonlinearities.

For this work, SO channel data measured between April 2018 and February 2020, spanning both hemispheres, were analyzed. HCl features should be observed in several orders (125 to 130), and orders 129 (2889 to 2921 cm1) and 130 (2920 to 2943 cm1), which have been regularly observed, have been used to detect HCl. These datasets represent in total 264 observations in which 36 are positive detections. A positive detection is a 5- retrieved VMR for which the weighted average of the bins is greater than 0.3 ppb at more than two tangent heights ( is the SD of the mean of retrievals from the four bins).

The HCl mixing ratio is retrieved by fitting the entire spectral range of either order 129 or 130. The temperature, pressure, and CO2 VMR are taken from the values predicted by the GEM-Mars model (56) for each altitude, taking into account the GDS (17). Computed spectra are convolved with an instrument line shape, and the forward model accounts for the effects of the AOTF and the grating. Retrievals are performed using an optimal-estimation approach and line-by-line radiative transfer code (ASIMUT) developed for planetary atmospheres (57). Retrievals are performed independently at each tangential altitude (11). Figure S3 shows examples of bin-averaged spectra and best-fit lines for orders 129 and 130 featuring HCl absorption lines.

D. C. Catling, M. L. Smith, M. W. Claire, K. J. Zahnle, paper presented at the EPSC, London, UK, 2013.

F. Lefvre, V. Krasnopolsky, The Atmosphere and Climate of Mars, R. M. Haberle, R. T. Clancy, F. Forget, M. D. Smith, R. W. Zurek, Eds. (Cambridge Planetary Science, Cambridge University Press, 2017), pp. 405432.

J. B. Burkholder, S. P. Sander, J. P. D. Abbatt, J. R. Barker, R. E. Huie, C. E. Kolb, M. J. Kurylo, V. L. Orkin, D. M. Wilmouth, P. H. Wine, Chemical Kinetics and Photochemical Data for Use in Atmospheric Studies: Evaluation Number 18, (Technical Report, Jet Propulsion Laboratory, NASA, 2015).

G. P. Brasseur, S. Solomon, Aeronomy of the Middle Atmosphere: Chemistry and Physics of the Stratosphere and Mesosphere (Atmospheric and Oceanographic Sciences Library, Springer Netherlands, ed. 3, 2005).

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Transient HCl in the atmosphere of Mars - Science Advances

How Old is the Ice at Mars North Pole? – Universe Today

On Earth, the study of ice core samples is one of many methods scientists use to reconstruct the history of our past climate change. The same is true of Mars northern polar ice cap, which is made up of many layers of frozen water that have accumulated over eons. The study of these layers could provide scientists with a better understanding of how the Martian climate changed over time.

This remains a challenge since the only way we are able to study the Martian polar ice caps right now is from orbit. Luckily, a team of researchers from UC Boulder was able to use data obtained by the High-Resolution Imaging Science Experiment (HiRISE) aboard the Mars Reconnaissance Orbiter (MRO) to chart how the northern polar ice caps evolved over the past few million years.

The research was conducted by Andrew Wilcoski and Paul Hayne, a Ph.D. student and assistant professor from the Laboratory for Atmospheric and Space Physics (LASP) at the University of Colorado Boulder. The study that describes their findings recently appeared in the Journal for Geological Research (JGR), a publication maintained by the American Geophysical Union (AGU).

For the sake of their study, Wilcosky and Hayne sought to determine the current state of the Martian North Polar Residual Cap (NPRC), which is vital to understanding the North Polar Layered Deposits (NPLD). Using the high-resolution images gathered by the HiRISE instrument, Wilcosky and Hayne examined the rough features of the NPRC which includes ripples and ridges of varying size and shape.

They then modeled the growth and recession of NPRC over time based on its interaction with solar radiation and how the rate of growth and loss is affected by the amount of atmospheric water vapor. What they found was that in addition to causing the formation of rough terrain (ripples and ridges) in an ice sheet, exposure to solar radiation will also cause ice to sublimate unevenly.

Basically, Mars axial tilt, which is responsible for it experiencing seasonal changes similar to Earth, also causes one side of these features to sublimate (the Sun-facing side) while the other does not. This has the effect of exaggerating these features, leading to pronounced ridges and valleys that become more pronounced as time goes on.

Overall, the model employed by Wilcoski and Hayne determined that the rough features observed by the MRO should measure 10 m (33 ft) in diameter and 1 m (3.3 ft) deep. Furthermore, their results demonstrated that as the features age, the spatial wavelength (the distance) between each ripple increases from 10 to 50 m (164 ft). As they state in their study:

Our results show that the size of mounds and depressions on the ice cap surface suggest that it took 110 thousand years to form these roughness features. Our results also suggest that the formation of features on the surface may depend on when water vapor is present in the atmosphere over the course of a year (e.g., summer or winter).

These results are consistent with the images taken by the HiRISE instrument of the Martian North Polar Residual Cap (NPRC). What they indicated is that the rough features observed around Mars northern polar ice formed within the last 1000 to 10,000 years, which provides scientists with a starting point for reconstructing the climate history of Mars.

Such is the nature of the Red Planet. Today, scientists have a pretty good understanding of the nature of the Martian landscape and how it changes throughout the year. They also have an idea of what it used to look like billions of years ago, thanks to impeccably-preserved surface features that indicate the past presence of flowing and standing water (rivers, streams, and lakes).

But the intervening period, where the climate transitioned from one to the other, thats where much remains to be learned. In the coming years, robotic missions could be sent to Mars for the sake of studying the ice sheets directly and maybe even return samples to Earth. In the next decade, as astronauts begin to set foot on Mars, the opportunity to explore the ice caps could also be possible.

Further Reading: EOS (AGU), JGR Planets

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How Old is the Ice at Mars North Pole? - Universe Today

Water heavily fractionated as it ascends on Mars as revealed by ExoMars/NOMAD – Science Advances

Abstract

Isotopic ratios and, in particular, the water D/H ratio are powerful tracers of the evolution and transport of water on Mars. From measurements performed with ExoMars/NOMAD, we observe marked and rapid variability of the D/H along altitude on Mars and across the whole planet. The observations (from April 2018 to April 2019) sample a broad range of events on Mars, including a global dust storm, the evolution of water released from the southern polar cap during southern summer, the equinox phases, and a short but intense regional dust storm. In three instances, we observe water at very high altitudes (>80 km), the prime region where water is photodissociated and starts its escape to space. Rayleigh distillation appears the be the driving force affecting the D/H in many cases, yet in some instances, the exchange of water reservoirs with distinctive D/H could be responsible.

Mars shows a scarred landscape carved by a wet past [e.g., (1)], yet it is not clear how much of this water ran across the Martian surface or for how long. The debate includes considerations of a wet and cold past scenario [e.g., (2)], wet and hot past [e.g., (3)], or hybrid models [e.g., (4)]. In many cases, these scenarios are stimulated by the strong geological record but depend highly on the assumed atmospheric states and escape considerations. Measurements of isotopic ratios and, in particular, the deuterium to hydrogen ratio (D/H) in water provide a powerful method to constrain volatile escape [e.g., (5)] and to track the transport of water between reservoirs (e.g., seasonal transport between the polar caps). Because the thermal Jeans escape rates for each isotope are different (larger for the lighter forms), over long periods, the atmosphere becomes enriched in the heavy isotopic forms. By mapping the current isotopic ratios, one can also test for the existence of different volatile reservoirs (e.g., polar caps and regolith) with distinct isotopic signatures (6).

The idea of distinct water reservoirs interacting during the water cycle was strengthened by the strong isotopic variations in the water column that were observed across the planet via ground-based astronomy (5, 7). Nevertheless, the D/H ratio is also heavily affected by climatological processes because the vapor pressures of HDO and H2O differ near the freezing point, making the condensation/sublimation cycle of the isotopologs sensitive to local temperatures, to saturation levels, and to the presence of aerosol condensation nuclei. This would lead to strong seasonal D/H gradients, while local orography and cloud formation would lead to longitudinal variability.

By performing high-resolution infrared spectroscopic observations across the entire planet, the ExoMars Trace Gas Orbiter (TGO) provides an unprecedented view of the three-dimensional structure and composition of the Martian atmosphere. Specifically, the NOMAD (Nadir and Occultation for Mars Discovery) (8, 9) instrument suite aboard TGO has the capability to provide vertical profiles and global maps of water (both H2O and HDO), water ice, and dust using high-resolution infrared spectroscopy. The vertical and seasonal trends in water vapor during the global and regional dust storms of Mars Year (MY) 34 were extensively presented (10), while the present work emphasizes the relationship between water abundance and the D/H ratio based on data acquired with the SO (solar occultation) channel of NOMAD between April 2018 (the start of science operations) and April 2019. This interval corresponds to Ls = 162.5 of MY 34 to Ls = 15.0 of MY 35 and included the global dust storm (GDS) that engulfed the planet in MY 34 (June to September 2018). A total of 219,464 individual SO spectra through the Martian atmosphere were collected during 1920 occultation events.

ExoMars TGOs near-polar orbit with up to 24 occultations per sol, shared between NOMAD and Atmospheric Chemistry Suite (11), permits high-cadence mapping of the variability of water and D/H over time. Sensitivity typically allows water mapping up to an altitude of ~100 km for the main isotopolog of water (H2O) and up to ~50 km for HDO and, thus, D/H (with a typical resolution of ~1 km), while high opacity from aerosols and airborne dust restrict the lower boundary to 5 to 10 km. The SO channel operates at wavelengths between 2.2 and 4.3 m (2325 to 4500 cm1) using an echelle grating, combined with an acousto-optic tunable filter (AOTF) and delivers a spectral resolving power of ~20,000. The width of each AOTF filtered order varies from 20 to 35 cm1, linearly increasing with the diffraction order number. The infrared channels (SO and nadir channel) of the NOMAD instrument are described in detail in previous works (1215), while a complete calibration using the in-flight data acquired before the science phase has been discussed in depth (16).

During an occultation, the SO instrument is pointed toward the Sun to observe the solar radiation as attenuated by the Martian atmosphere at different altitudes, enabling an investigation of the atmospheric vertical structure. On a typical occultation, five or six different diffraction orders are sampled at 1-s intervals, with H2O sampled in two or more diffraction orders and HDO in one of them, ultimately allowing quantification of D/H for almost all NOMAD occultations (see example spectra in Fig. 1). The possibility to access different absorption bands of water is of great benefit to achieve measurement accuracy throughout a vast range of altitudes since absorption regimes vary with the observed atmospheric column. For instance, strong fundamental bands of H2O (such as the v3 band at 2.7 m, orders 168 to 170) probe water up to 120 km but become saturated at ~50 km, while the weaker 22 band at 3.3 m (orders 133 to 136) probes deeper into the atmosphere without saturation.

The observations were taken during the GDS and show that the two bands (1 of HDO and 22 of H2O) have similar opacities and, therefore, comparable curves of growth and altitude sensitivity.

We derived H2O and HDO slant column densities from the resulting spectra by using Goddards Planetary Spectrum Generator (PSG) (17), which is based on an optimal estimation approach (18), modified with an extra regularization parameter (19, 20). For Mars, PSG ingests a specific line compilation for water and its isotopologs, tailored for a CO2-rich atmosphere (21, 22). The derivation of molecular mixing ratios does depend on the assumed pressure/temperature profiles, and in particular, the local atmospheric density and temperature can vary during perihelion season, depending on the intensity of heating introduced by dust present in the atmosphere. Because portions of the dataset were acquired during the GDS, the a priori atmospheric state has to be representative of those specific conditions. We calculated that using the Global Environmental Multiscale (GEM)Mars model (23, 24) and a specific dust storm scenario that reproduces the dust state of the atmosphere during MY 34. The properties of the GEM-Mars GDS model during the storm differ substantially from the average climatology of the Mars Climate Database (v5.2) (25), with temperature deviations as large as 30 K modeled in the middle atmosphere (fig. S4). The largest discrepancies are found in the southern hemisphere, where dust concentrations are greater during the GDS. The dust abundance or the assumed aerosols profiles do not affect the H2O and HDO SO retrievals directly (only when the atmosphere is fully optically thick). Dust will tend to heat the atmosphere, and that may reflect in enhanced partition functions, which ultimately affect the retrieved molecular densities. On the other hand, this effect is particularly small for the retrieved D/H since both partition functions vary similarly to temperature, so this systematic effect is removed when computing D/H.

To compute a single molecular profile per occultation, measurements are first collected to form a single dataset colocated in altitude (typically one to two orders for H2O and one to two orders for HDO) and then aggregated by a weighted mean. Each molecular retrieval is assumed to be independent from the nearby altitude retrievals, with the resulting uncertainty also including the standard deviation of the measurements (see figs. S6 and S7). The D/H ratio is determined using the same approach: For each occultation and altitude, the D/H is computed using the weighted averages of H2O and HDO. Uncertainties were computed using standard optimal estimation statistics that are further corrected for the quality of the residual spectra (chi-square of the fit). Measurements from several orders and computation of uncertainties of D/H were performed using standard error propagation methods [see also (5, 9)].

The retrievals were organized by season and latitude to investigate the main processes acting on water and D/H. As shown in Fig. 2, the water vapor abundances change markedly across the year, with D/H also showing important changes. Previous measurements of water columns [e.g., (2630)] also report great seasonal, temporal, and spatial variability, with strong enhancements during the summer hemisphere as reported here. The seasonal variability reported here should be viewed with caution since the orbit of ExoMars causes seasonal and latitude changes to be convolved (Fig. 2, top). Note that these are local D/H values at a specific altitude (not of the column), and they can be only understood in the context of the local climatology at this specific altitude/latitude/longitude/season.

Only H2O values with sigmas lower than 15 parts per million by volume (ppmv) and D/H values with sigmas lower than 0.8 VSMOW are shown (point-by-point error bars are presented in fig. S7). Because of the ExoMars/TGO orbit, there is an intrinsic relationship between the seasonal and latitudinal sampling for the occultations, and the latitude subpanels indicate which latitudes are sampled during a particular instance. Water is observed to reach the upper regions of the atmosphere (>80 km) during indicated events: (i) during the GDS, (ii) during the regional dust storm, and (ii) during southern summer, in which we observe a localized upper atmosphere water excess.

Consistent with earlier studies of dust storms (10, 31), we found that water vapor abundances in the middle atmosphere (40 to 100 km) increased substantially during the GDS (June to mid-September 2018) and the regional dust storm of January 2019. In particular, water vapor reaches very high altitudes, at least 100 km, during the GDS. A General Circulation Model simulation explained that dust stormrelated increases in atmospheric temperatures elevate the hygropause, hence reducing ice cloud formation and so allowing water vapor to extend into the middle atmosphere (24). We confirm that (i) water vapor also reaches very high altitudes during the southern summer solstice, independently of dust storms [see lower dust content during this period as reported in (32)] and (ii) that water drops to very low values at high/low latitudes and close to equinox with the hygropause subsiding to a few scale heights. With regard to D/H, we observe the following distinct features: (i) the D/H ratio is typically ~6 VSMOW (Vienna Standard Mean Ocean Water) in the lower atmosphere, (ii) the D/H ratio decreases with altitude, as observed similarly on Earth (22), and (iii) the D/H ratio is low (2 to 4 VSMOW) at high/low latitudes and close to equinox where H2O is low.

Within half an MY, we observed three instances (the GDS, southern summer, and the regional dust storm) of water vapor reaching the upper atmosphere, where it can be readily photolyzed (24), bypassing the traditional H2 diffusion limitations on water escape rates (33). The D/H ratio is probably quite low at these high altitudes if we attempted to extrapolate our D/H values to 70 to 80 km from the low/middle atmosphere (50 to 60 km), yet photolysis, vertical transport, and other processes may lead to great variability at these altitudes. On Earth, mesospheric D/H measurements show strong variability (34), which has been attributed to the differential photolysis rates of HDO and H2O combined with atmospheric transport and CH4/CH3D photochemistry. For the lower atmosphere, the decrease of the D/H with altitude can be explained, as on Earth, by Rayleigh fractionation (22). The fractionation in the troposphere of Earth has been shown to be also strongly dependent on atmospheric dynamics [e.g., see convective/subsiding results in (35) and formation of clouds and atmospheric microphysics in (36)], resulting in highly variable deuterium enrichments with respect to altitude, time, and position on the planet [e.g., (37, 38)]. These may explain the localized behavior and variability in the D/H ratio observed across Mars, and it is consistent with the column variability observed in (5).

To explore the 3D structure of the water cycle and the D/H signatures, we aggregated the data into seasonal periods and computed latitude versus altitude plots of water vapor and D/H (Fig. 3). These plots show a marked variability of the vertical profiles of water and D/H, with clear and defined latitudinal structures. As also shown in (10), the increase of the water vapor abundances at higher altitudes is remarkable for the global (Ls = 190 to 210) and regional dust storm (Ls = 320 to 330), yet this excess water is only confined to equatorial and mid-latitudes (<60). Although the atmosphere is filled with water to high altitudes during these times, the D/H remains relatively low (4 to 5 VSMOW) and increases to ~6 VSMOW only at high latitudes (away from the subsolar point) and low altitudes. In principle, this is expected and could be an indication of Rayleigh fractionation and cloud formation (9), where D/H is actually decreasing with altitude, but it is only measured with sufficient signal-to-noise ratio (low opacities) at high altitudes (>40 km) in mid-latitudes and at low altitudes (10 to 40 km) in high latitudes.

Only H2O values with sigmas lower than 15 ppmv and D/H values with sigmas lower than 1.5 VSMOW are shown. The panels clearly show the evolution of the water cycle across these complex events, revealing marked changes in the water and D/H distributions across the events. The sparsity of valid D/H datasets considering this fine temporal sampling does not allow us to fully capture every detail of the latitude by altitude variability, yet two points are clearly observed: (i) The water released from the southern polar cap has a distinctive 6- to 7-VSMOW enrichment in D/H, and (ii) during southern fall (Ls 300 to 320 and Ls 330 to 360), the hygropause is compacted in the southern hemisphere, leading also to very low D/H at these latitudes and season.

The injection of southern polar cap water with enhanced D/H is clearly seen as southern spring progresses to summer. Between Ls = 270 and 300, we see water vapor increasing in the southern hemisphere and also in altitude as we approach the polar latitudes [labeled in Fig. 2 as aspirator (from the Latin word aspire to rise, climb up)]. The D/H remains high (>6 VSMOW) for most of this water (probably coming from the seasonal southern polar cap) and decreases to <4 VSMOW at higher altitudes. Fractionation is also present at this season, associated with a more compact hygropause in the colder/winter hemisphere and a more compact D/H profile. As we move to southern fall (Ls = 300 to 320), the water may have been transported to equatorial latitudes, which is then puffed into higher altitudes during the regional dust storm (Ls = 320 to 330). During the regional storm, water reaches only 60 km in altitude, in comparison to 80 to 100 km observed during the GDS. Water abundance then collapses to low values and at low altitudes during southern fall (Ls = 330 to 360) and early northern spring (Ls = 360 to 370, MY 34). The D/H information during this period is inconclusive since water is confined to low-altitude layers of the atmosphere, where long atmospheric path lengths prevent observations of HDO with sufficient sensitivity due to aerosol extinction. During this season, we do observe low D/H values in the southern hemisphere and very low values at low altitudes.

Multiple reservoirs have been identified to account for the current inventory of water on Mars, ranging from the observable polar layered deposits (39, 40) to ice-rich regolith at mid-latitudes (41, 42), near-surface reservoirs at high latitudes (43), and subsurface reservoirs, as implied by gamma ray and neutron observations (44). If each of these reservoirs has a distinct isotopic content, then the signature of the exchange between these reservoirs should be present in the observed atmospheric D/H ratio variation. The outstanding question is whether each reservoir has or should have a distinct isotopic signature. The fact that Mars has had marked variations in its obliquity (45), changing from ~45 to 15 in the last million years, would suggest that the polar caps are relatively new and that all the water reservoirs should have been mixed within the last 10 million years. Considering that it takes billions of years for notable changes in the D/H ratio to take effect, the different reservoirs may have the same isotopic signature, yet this hypothesis assumes that all labile water is mixed by the hydrological cycle. A testable way to prove this hypothesis would be to ultimately probe the water D/H in the polar caps below the seasonal layers. We then ask, is the variability that we observe related to different reservoirs?

As on Earth (46), D/H on Mars shows great variability in time and space, consistent with previous column integrated reports in (5, 47). Observations using SOFIA (Stratospheric Observatory for Infrared Astronomy) at thermal wavelengths (48) do also report variability yet much more subdued. Thermal observations are more affected by the assumed temperature profiles and thermal contrast, and the spatial resolution of SOFIA observations is typically only four to five pixels across Mars disk; however, it is interesting to note this difference between SOFIA and other results. In particular, there may be an annual element to this hemispheric variability of the observed D/H column. Strong isotopic anomalies are typically observed at regions with strong temperature/water gradients, like the polar caps, and these are typically hard to capture and sample at moderate spatial resolutions from the ground.

In many cases, the observed variations of the D/H across seasons and with altitude revealed by our work could be attributed to Rayleigh fractionation and cloud formation (32), with the D/H decreasing with altitude and dropping or decreasing at the edge of the hygropause. In the zonal mean Fig. 3, the seasonal water being added from the southern polar cap during southern summer (Ls = 210 to 250 and 270 to 300) has a ~6- to 7-VSMOW value, consistent with the column values measured in (5) for the northern pole water. This would perhaps mean that the two main reservoirs of water on Mars, the polar caps, share a common value of D/H, yet the south polar cap only has seasonal water ice, not permanent. The lower values in D/H observed during southern fall (Ls = 300 to 320 and 330 to 360) at the southern latitudes would imply that a large fraction of the HDO was sequestered. This could be associated to be a rapid collapse of the hygropause at these latitudes, which leads to a steep Rayleigh fractionation condensation profile. The existence of water ice clouds during this period and season (31, 32) is consistent with this view.

Further interpreting the results, in particular, the concept of multiple reservoirs of water with a distinctive D/H and water escape would require detailed comparisons with a highly parameterized weather and climate model. The model would need to have a comparable prescription of the water and aerosol distribution and to have a realistic heterogenous water fractionation model to fully capture the observed D/H variability and advance current models (4951). The ultimate question is then what is the representative D/H of labile water on Mars right now? If we assume that the observed fractionation is driven mainly by Rayleigh distillation, then the observed maximum D/H values of 6 to 7 VSMOW observed in this work are then descriptive of the truly intrinsic water D/H when both isotopologs are fully vaporized. This value is consistent with previous findings as reported above and would further establish that Mars has lost a substantial amount of water (>137-m global equivalent layer) (5). The fact that we observe three instances during a single MY where water is brought to the upper regions of the atmosphere (>60 km; Figs. 2 and 3) would provide the means for this escape to take place.

W. Darling, G, A. H. Bath, J. J. Gibson, K. Rozanski, Isotopes in water, in Isotopes in Palaeoenvironmental Research, M. J. Leng, Ed. (Springer, 2006), pp. 166.

K. Stamnes, G. E. Thomas, J. J. Stamnes, Radiative Transfer in the Atmosphere and Ocean (Cambridge Univ. Press, 2017).

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Water heavily fractionated as it ascends on Mars as revealed by ExoMars/NOMAD - Science Advances