Earth System Remote Sensing/Earth Dynamics Observatory University of Arizona Cluster Hire Announcement

The University of Arizona announces coordinated hiring of five tenure-track or tenured faculty positions in Earth system remote sensing to establish the Earth Dynamics Observatory (EDO) to respond to global challenges in Earth and environmental science, planetary science, and hazards and resource assessment.

EDO will combine unique mission operations and planetary science capabilities of the internationally recognized Lunar and Planetary Lab with remote sensing research in leading natural science programs including Geosciences, Hydrology and Atmospheric Sciences, the School of Natural and Resources and the Environment, and the Institute of the Environment, with instrument development and calibration through UA's renowned Colleges of Science, Optical Sciences, and Engineering. EDO faculty will contribute to interdisciplinary research and educational programs oriented around remote sensing and Earth and planetary change, with the goal of developing instruments, deploying missions, and leading new research in applications of remote sensing.

We welcome applications for the first five EDO positions focused in five areas. For all positions, scientists may seek appointments in one or several Departments and Colleges within the University, depending on the research areas and interests of the scientist and the promotion of mission- and science-oriented objectives of EDO.

Appointees will be expected to contribute to innovative and quality teaching, advising, and mentoring at the graduate and undergraduate level, provide opportunities for student engagement in research, internship, externship, and professional training, participate in service and outreach, and promote the UA's goals for broad representation among its students and workforce. EDO is seeking individuals who promote diversity in research, education, and outreach, and who have experience with a variety of collaborative, teaching, and curricular perspectives.

At the University of Arizona, we value our inclusive climate because we know that diversity in experiences and perspectives is vital to advancing innovation, critical thinking, solving complex problems, and creating an inclusive academic community. We translate these values into action by seeking individuals who have experience and expertise working with diverse students, colleagues and constituencies. Because we seek a workforce with diverse perspectives and experiences, we encourage minorities, women, veterans, and individuals with disabilities to apply. As an Employer of National Service, we also welcome alumni of AmeriCorps, Peace Corps, and other national service programs.

Instrument/Mission Leadership:We seek a scientist with experience in instrument and/or mission development and leadership in Earth remote sensing to coordinate large-scale collaborative projects across a variety of platforms (airborne, UAV, satellite), methods (multi/hyperspectral, radar, laser, gravity, etc.), and applications (e.g., atmospheric composition/properties, Earth surface, land cover, sea-surface, cryosphere, groundwater, etc.). The position is open-rank. In addition to promoting interdisciplinary collaboration across campus and with federal, regional, and industry partners, the scientist will also contribute to training students and researchers in remote sensing, and serve remote-sensing related needs of regional resource stakeholders. Inquiries should be directed to Jonathan Overpeck, jto@email.arizona.edu. Candidates should apply for position number F20158.

Remote Sensing Land-Water-Climate/Geospatial Analysis: We seek a scientist with expertise in remote sensing, modeling, and data analysis to address challenges in land surface, water cycle, resource, and hazards assessment using active and passive source methods, multi- and hyperspectral data, LiDAR, and other technologies. Experience with advancedspatial-temporal modeling and geospatial analysis related to environmental change and water in arid environments is expected. The scientist will engage researchers and students in interdisciplinary research and student training across Earth and environmental programs and curricula, and lead and collaborate on federal, industry, and public projects. Inquiries should be directed to Stuart Marsh, smarsh@email.arizona.edu. Candidates should apply for position number F20163.

Atmospheric remote sensing: Observing systems, encompassing a wide range of platforms from ground-based to satellites and measurement instruments from radar to chemical sensors, are key in our ability to understand, predict, assess, and mitigate changes in the Earth system. We seek a scientist with expertise in atmospheric remote sensing especially in the following areas: (1) passive and active remote sensing of the atmosphere (e.g., precipitation, clouds, water vapor, aerosols, and trace gases); (2) development and application of remote sensing retrieval algorithms and methods; (3) algorithm development and application of dual-polarization Doppler radar measurements; and (4) data assimilation. Inquiries should be directed to Xubin Zeng, xubin@atmo.arizona.edu. Candidates should apply for position number F20162.

Comparative planetology: We seek a scientist in the field of remote sensing of planetary surfaces, atmospheres, and/or interiors with relevance to multiple planets (including exoplanets) or solar system objects and to astrobiology, to provide context for understanding the Earth. Experience in field and lab work and theory are also desirable. The scientist will have expertise in planetary science and observing techniques to a) develop instrumentation and techniques and lead experiments for planetary science (including Earth), and b) provide perspective on the implications for Earth of knowledge about other planets and vice versa. Inquiries should be directed to Tim Swindle, tswindle@lpl.arizona.edu. Candidates should apply for position number F20164.

Satellite Geodesy: We seek a scientist using modern space geodetic techniques to understand Earth properties across a range of geophysical, hazards, and resource applications. Examples include study of Earths gravity field, GPS, InSAR, and LiDAR imaging, radar altimetry, and other methods to probe Earths surface and interior to understand earthquakes, volcanoes, tsunamis, plate tectonics, mantle flow, glacier dynamics, sea level, and/or Earths rotational dynamics. This scientist will develop collaborative explorations into interconnected solid and fluid Earth systems for basic science, increase our ability to monitor Earth changes for resources and hazards assessment, strengthen our ability to compete for funding from external agencies and industry, and help define scientific objectives of future missions. Inquiries should be directed to Rick Bennett, rb0@email.arizona.edu. Candidates should apply for position number F20165.

Candidates can apply for all positions at http://www.uacareers.com, using the specific position numbers listed above.

Review of applications will begin 9 November 2015, and positions will remain open until filled.

Above: Photos of the Santa Catalina Mountains on Tucson's northern edge (and links to photo sources). Left: Cathedral Pk from Sabino Canyon. Middle: Snow above Bear Canyon. Right the Santa Catalinas, from tucsonhikes.wordpress.com.

Last modified 12 September 2015

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Earth Dynamics Observatory at the University of Arizona

Good morning everyone. My name is Professor Michael Andrews. On behalf of myself and my colleagues, I would like to welcome you to Extrasolar Planetology, which is a new class being offered by the Astronomy Department this year.

About twenty-five years ago, there was no solid proof that other planets existed beyond our solar system. Most astronomers at that time felt that planets had to be out there, but they could not see them or prove they were there. Why? Simply put, planets are small and space is vast. Imagine trying to see a pea with a telescope from a hundred miles away, and you'll understand how hard it is to find planets that are light years distant.

Clearly, something changed, for we now have a class called Extrasolar Planetology. What changed? Well, mainly, instruments got better and sophisticated telescopes were put into space. As a result, astronomers began to find the proof that they had lacked before.

The very first good evidence for the existence of other planets came from observations of 'wobbling' stars. Using their high-tech instruments and space-based telescopes, astronomers found that some stars wobbled as they moved through space. What could be causing this the astronomers wondered? And then Eureka! The only likely explanation seemed to be that these stars were being affected by the gravity of unseen orbiting companions. In other words-planets!

And now, if you would please turn off the lights, I would like to show you some slides of a few of these wobbling stars.

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Unit 37: Short Talk - Planetology - 1-Language

FSC History

The United States Geological Survey (USGS) Flagstaff Science Campus (FSC) houses science centers and research teams of the USGS that have a diverse range of scientific expertise. The late Eugene Shoemaker established the Astrogeology Branch of the USGS in Flagstaff in 1963, as a research facility for the new science of planetary geology. Flagstaff's clear air and high elevation made it a desirable location for telescope observations of the Moon and planets, and nearby Meteor Crater was a superb training ground for the Apollo astronauts. There and in the volcanic fields surrounding Flagstaff, astronauts tested equipment and were taught to look at the Moon through the eyes of a geologist.

While the initial focus of the FSC was lunar and planetary studies, other USGS groups began to migrate to the campus in the 1960s through the 1990s. Scientific collaboration among the various scientists located at the FSC provide one of the most unique USGS campuses in the country. The expertise of FSC scientists and collaboration opportunities provide the ability to address science issues related to water, ecosystems, climate and land-use change, energy and minerals, environmental health, and planetary exploration and study.

FSC staff provides outreach to other science organizations, schools, and to the general public. Scientists provide brown bag lectures on campus and other locations in Flagstaff. The public can take self-guided tours of FSC facilities and science displays. Also, FSC staff participates in Flagstaffs annual Festival of Science.

For more information about FSC outreach activities, please contact Greg Vaughan (gvaughan@usgs.gov, 928-556-7006)

The Flagstaff Remote Sensing Science Consortium (FRSSC, pronounced Frisk) includes scientists and other professionals at the USGS Flagstaff Science Campus (FSC) who develop and apply remote sensing techniques and methods in support of USGS science priorities and societal needs. Visit the FRSSC web page to learn more!

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USGS Flagstaff Science Campus - Public Page

New data from NASA's Dawn spacecraft suggest varied origins for tantalizing gleams on the dwarf planet's surface

The surface of the dwarf planet Ceres (shown here) has fewer large craters than researchers expected. Credit:NASA/JPL-Caltech/UCLA/MPS/DLR/IDA

Not all of the puzzling bright spots on the dwarf planet Ceres are alike. The closest-yet images of the gleams, taken from 45,000 kilometres away, suggest that at least two of the spots look different from one another when seen in infrared wavelengths.

The Hubble Space Telescope spied many of the bright spots from afar years ago, but the observations from NASA'sDawn spacecraftwhich began looping around Ceres on March 6are the first at close range. The images were released on April 13 in Vienna, Austria, at a meeting of the European Geosciences Union.

Scientists say that the bright spots may be related to ice exposed at the bottom of impact craters or from some kind of active geology. They glimmer tantalizingly in a new full-colour map of Ceres, obtained in February but released at the conference. The map uses false colours to tease out slight differences on the otherwise dark surface of Ceres.

This is the first idea of what the surface looks like, said Martin Hoffmann, a Dawn scientist from the Max Planck Institute for Solar System Research in Gttingen, Germany.

Dawn is beginning to sharpen its view of the bright spots as it gets closer to Ceres. The new infrared images compare Spot 1, near Ceres' equator, with a pair of bright spots collectively known as Spot 5. Some scientists have speculated that the latter could belinked to an icy plume.

Spot 1 appears darker in images from Dawn's infrared spectrometer, said Federico Tosi, a Dawn scientist at the Institute for Space Astrophysics and Planetology and the Italian National Institute for Astrophysics in Rome. That suggests that the area is cooler than the rest of the dwarf planet's surface, supporting the idea that the spot is made of ice.

But for some reason Spot 5the brightest feature seen on Dawndoes not show up in infrared images. One possibility is that we still dont have enough resolution to see it in the proper way, said Tosi.

Dawn has also shown that some parts of Ceres are pockmarked by impact craters, while other regions seem smooth. So far there seem to be fewer large craters on Ceres than expected, says the mission's principal investigator, Christopher Russell of the University of California, Los Angeles.

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Mystery of Ceres's Bright Spots Grows

My eve online planetology harvesting scheme
sorry for low-quality (i have ADSL internet and can #39;t upload huge videos).

By: Ivan Belotserkovsky

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My eve online planetology harvesting scheme - Video

Comparative Planetology

In the 1970s, space probes radically increased our data on other planets in our solar system from space probes. Researchers were able to use this information to compare and contrast the different planets, looking for processes that work universally across planets with similar conditions. According to this technique, called comparative planetology, we can learn more by looking for the unifying principles different planets share, rather than by studying each planet as an unrelated system.

The planets in our solar system all formed from essentially the same stuff, yet they are now strikingly different in appearance and surface composition. To understand how this differentiation occurred we must look at both external processes (such as the delivery of water by comets) and internal processes (such as volcanism). The comparison of greenhouse warming on Venus, Earth, and possibly Mars, is one example of a process that occurs in different levels on different worlds. The presence of life and liquid water is another example they are present on Earth, but our two closest neighbors, Venus and Mars, currently lack either. Nature has performed various experiments for us, placing planets of different sizes at different distances from the Sun. We can compare the results of the experiments to learn more about how planets work in general, and especially about how the Earth itself works. Life, just like volcanism, effects our planets atmosphere, chemistry, and surface. Studying other, simpler, systems can help us understand the Earth more completely.

There are some simple, general rules we can derive from this method that helps us understand planets. Here are some examples:

The tenets of comparative planetology are all based on simple physical principles related to gravity, chemistry, and the kinetic theory of matter. Since we have evidence that these physical properties are universal, its a good bet that these rules apply to planets beyond the solar system, too. The exciting idea that we can predict the properties of yet-undiscovered planets is an example of the long reach of the scientific method.

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Comparative Planetology - Teach Astronomy

Astronomy - Ch. 7: The Solar Sys - Comparative Planetology (28 of 33) Asteroids 1
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Astronomy - Ch. 7: The Solar Sys - Comparative Planetology (28 of 33) Asteroids 1 - Video

The search for geothermal energy under the dormant Hualalai volcano is moving forward.

A University of Hawaii researcher has asked the state Board of Land and Natural Resources for a geothermal exploration permit to conduct a noninvasive geophysical study of the west rift zone of Hualalai, just north of Kailua-Kona.

The project is funded by the U.S. Department of Energy and the state Department of Land and Natural Resources, researcher Nicole Lautze, with the Hawaii Institute of Geophysics and Planetology, said in her application. She did not return a phone message left at her office by press time Monday.

The Land Board is scheduled to consider the application Friday. The meeting is held in Honolulu and begins at 9 a.m.

Lautze said in her application that the Hualalai exploration is the first exploration permit in what will be an overall effort referred to as the Geothermal Resources Exploration Plan for Hawaii.

Researchers plan to conduct their surveys on nine parcels of land, all zoned agriculture. Theyve gotten permission from the landowners, which are the state, Kamehameha Schools, Makalei Golf Club, the Queen Liliuokalani Trust and Palani Ranch.

Researchers will use a standard technique called magnetotelluric survey that maps the electrical conductivity of rocks at depths from several hundred feet to as much as 20,000 feet below the surface.

The vast majority of developed geothermal systems in the world are located in regions where water can flow naturally through the heated rock formations, Lautze said in her application. Being able to identify the subsurface heat source and fractured zones allows us to begin to address some of the problems of geothermal exploration and development.

The system uses antennas and electrodes to measure naturally occurring, very low frequency electromagnetic waves. The apparatus does not generate electrical signals or transmit energy, Lautze said.

The islands geothermal production is currently limited to one 38-megawatt power plant, Puna Geothermal Venture, outside Pahoa.

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Hualalai geothermal study planned

Astronomy - Ch. 7: The Solar Sys - Comparative Planetology (29 of 33) Asteroids 2 (Composition)
Visit http://ilectureonline.com for more math and science lectures! In this video I will examine the compositions of asteroids. Next video in this series can be seen at: http://youtu.be/tQ6PcoOrrr0.

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Astronomy - Ch. 7: The Solar Sys - Comparative Planetology (29 of 33) Asteroids 2 (Composition) - Video

The Hawaii Institute for Geophysics and Planetology has developed a website to make data on groundwater and geothermal resources accessible to the public.

The objective for the website is to bring together UH research with data on groundwater and geothermal resources that is collected by the Hawaii Department of Land and Natural Resources (DLNR) and Department of Health (DOH), University of Hawaii at Mnoa Geochemist Donald Thomas said.

According to Thomas, groundwater data goes back 100 years or more and is not very accessible to the public. The website formats the past and current data that is more easily accessible for people who want to learn more about geothermal resources.

Ultimately what we would really like is to have a system were people can go in and understand more about the groundwater system, Thomas said.

He added the first phase of the Hawaii Groundwater and Geothermal Resource Center (HGGRC) website is to analyze the data to see how sources of groundwater have changed over time due to climate change or urban development and how they should be managed in the future.

Both the data and information on the website have been generated by Hawaii Institute of Geophysics and Planetology scientists since 2010.

The HGGRC website provides searchable map displays that show what is to come for groundwater and geothermal energy data.

Humuula GroundwaterResearch Project

One project connected to the website, the Humuula Groundwater Research Project, focuses on researching the groundwater resources on Hawaii Island.

The projects researchers will drill two holes on the grounds of the Phakuloa Training Area (PTA), in the center of the island, to depths of 6000 to 6500 feet from the surface. The goal is to reach the point where the fresh groundwater and the oceans salt water meet and take rock core samples for future scientific study.

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UH website makes groundwater research public

Astronomy - Ch. 7: The Solar Sys - Comparative Planetology (31 of 33) Comets 2
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Astronomy - Ch. 7: The Solar Sys - Comparative Planetology (31 of 33) Comets 2 - Video

Astronomy - Ch. 7: The Solar Sys - Comparative Planetology (33 of 33) Water in the Solar System
Visit http://ilectureonline.com for more math and science lectures! In this video I will explain where the water on planets and moons in our Solar System com...

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Astronomy - Ch. 7: The Solar Sys - Comparative Planetology (33 of 33) Water in the Solar System - Video

Astronomy - Ch. 7: The Solar Sys - Comparative Planetology (32 of 33) Impact Craters
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Astronomy - Ch. 7: The Solar Sys - Comparative Planetology (32 of 33) Impact Craters - Video

PROJECT CAMELOT : KAMERAN FALLY - PLANET X ASTRO-PLANETOLOGY
This is an interview with Kameran Fally, banker, physicist, religious scholar and political advisor to top levels of the British and Iraqi governments. GO TO : http://projectcamelotportal.com...

By: Project Camelot

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PROJECT CAMELOT : KAMERAN FALLY - PLANET X & ASTRO-PLANETOLOGY - Video

Astronomy - Ch. 7: The Solar Sys - Comparative Planetology (26 of 33) Atmosphere 1
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Astronomy - Ch. 7: The Solar Sys - Comparative Planetology (26 of 33) Atmosphere 1 - Video

Astronomy - Ch. 7: The Solar Sys - Comparative Planetology (27 of 33) Atmosphere 2
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Astronomy - Ch. 7: The Solar Sys - Comparative Planetology (27 of 33) Atmosphere 2 - Video

Saturn is, of course, famous for its rings, but in our solar system there are actually four planets with ring systems of one size or another. Every gas giant in our solar system has a ring that is to say, right now the evidence suggests that everygas giant could have a ring. As mankind begins to look directly at the planets of the universe outside our own solar system, any universal rule of that sort will be vitally important. Now, astronomers are gearing up to start countinggas giants outside our solar system, as a new technique allows identification ofplanetary rings from light-years away.

The technique is as simple as could be, and could even be applied to existing readings to get new information outofold studies. Right now, planets are identified mostly by looking at the change in luminosity of their parent star when the planet moves between that star and the Earth; these readings are called transits. The silhouette is recorded as a rather abstract graph, and if the graph shows thata planet blocks more light from itsstar than it ought to, given predictions for its size, there are two basic possibilities: Either your predictions were wrong in some way, or the objects apparent size is expanded somehow say, withrings.

The researchers want to go back at look at numerous results that earlier studies discarded as false positives tosee whether they might have been planets encircled by rings. If they find that their work can explain historical results more accurately than current theory (or at all), astronomers might end up buildinga list of previously abandoned celestial bodiesto revisit.

Ringed exoplanets came to prominence recently, as a so-called super-Saturn was found with rings many times the size and mass of Saturns (artists rendition at top of page). The actual identity of J1407b is not quite known, however; it could be a dwarf star, and the rings still-forming planets. Additionally, while this method can provethe existence of rings, it cant prove the non-existence of them. In other words, just because this technique doesnt see an expansion in the transit readings, doesnt mean there arent rings. All it really means is that if there are rings, they must be quite thin.

The light-blocking effect changes based on the angle of the rings to the Earth.

Thus, this techniquecant be used in any case where astronomers cant get a second size reading by adifferentmethodof measurement than transit. Without that second measurement, theres no way to tell if the planets transit is blocking more light than it ought to.

Why should astronomers care about rings, specifically? Firstly, because they couldprovide a window into the past of whicheversolar system we end up finding them within. Rings can be very diverse in their makeup and, more importantly, often let a fair amount of light through. Astronomers are great at working with partially blocked light just recently, insight into planetary atmospheres and ever weather patterns was gleaned from light leaking around the edges of a distant planet.

Rings are also often associated with moons. Ancient moon-planet collisions are one possible source of planetary rings, but moons also sometimes enforce the edges and details of a planetaryring. By orbiting in asimilarplane tothe ringsthemselves, a large body like a moon can sweep up any small particulate matter simply by running into it. So far there have been no exo-moons found, but perhaps a ringed system could alert astronomers to a good potential candidate.

Exo-planetologyis undoubtedly the fastest-growing area of astronomy. The Kepler planet-hunter was NASAs very first attempt at finding planets by their transit signatures, and it found thousands. Now, the next generation transit finder, the Transiting Exoplanet Survey Satellite (TESS, is preparing to launch in 2017 and continue that quest. If exo-rings do end up being a major source of interest for astronomers, TESS is specifically the satellite that will be used tocapture them.

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The next frontier in planet science: exo-rings

Bernard Ray Hawke, director of the Pacific Regional Planetary Data Center (PRPDC), is dead at 68. He passed away in his sleep at Straub Hospital on Jan. 24.

A member of the University of Hawaii since 1978, Hawke initially joined as a planetary geologist and later became part of the Hawaii Institute of Geophysics and Planetology in 1983.

Hawke is noted for his research of collecting measurements of color at high resolution of small spots on the Moon, lunar geology, planetary photogeology and the cratering processes. His studies contributed to the understanding of the geological evolution of the lunar crust.

"He spent many hours at Hawaiis Mauna Kea Observatory, diligently working to make certain that data for the correct spot on the Moon was being acquired," saidPaul D. Spudsin his remembrance of the former planetary scientist.

Born in Louisville, Kentucky, in 1946, Hawke served in the army in 1970-71 and later analyzed lunar regolith chemistry as a Masters student at the University of Kentucky. He used a technique that would later be adopted "to decipher the geological history of the Apollo landing sites."

He later studied at Brown University where he earned another M.S. and a Ph.D in geological studies.

Hawke is survived by his brother Stephen, Stephens wife Nancie, and their children David and Michael of Columbia, Missouri.

A memorial gathering will be held in the Pacific Regional Planetary Data Center (POST 544) on Sunday, February 15 at 3 p.m.

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UH planetary director B. Ray Hawke dead at 68

Astronomy - Ch. 7: The Solar Sys - Comparative Planetology (25 of 33) Chemical Composition 2
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Astronomy - Ch. 7: The Solar Sys - Comparative Planetology (25 of 33) Chemical Composition 2 - Video

Astronomy - Ch. 7: The Solar Sys - Comparative Planetology (18 of 33) Planet Rotational Period
Visit http://ilectureonline.com for more math and science lectures! In this video I will discuss the various rotational periods of the planets in our Solar S...

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Astronomy - Ch. 7: The Solar Sys - Comparative Planetology (18 of 33) Planet Rotational Period - Video