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Planetary science – Wikipedia

Planetary science or, more rarely, planetology, is the scientific study of planets (including Earth), moons, and planetary systems (in particular those of the Solar System) and the processes that form them. It studies objects ranging in size from micrometeoroids to gas giants, aiming to determine their composition, dynamics, formation, interrelations and history. It is a strongly interdisciplinary field, originally growing from astronomy and earth science,[1] but which now incorporates many disciplines, including planetary geology (together with geochemistry and geophysics), cosmochemistry, atmospheric science, oceanography, hydrology, theoretical planetary science, glaciology, and exoplanetology.[1] Allied disciplines include space physics, when concerned with the effects of the Sun on the bodies of the Solar System, and astrobiology.

There are interrelated observational and theoretical branches of planetary science. Observational research can involve a combination of space exploration, predominantly with robotic spacecraft missions using remote sensing, and comparative, experimental work in Earth-based laboratories. The theoretical component involves considerable computer simulation and mathematical modelling.

Planetary scientists are generally located in the astronomy and physics or Earth sciences departments of universities or research centres, though there are several purely planetary science institutes worldwide. There are several major conferences each year, and a wide range of peer-reviewed journals. In the case of some exclusive planetary scientists, many of whom are in relation to the study of dark matter, they will seek a private research centre and often initiate partnership research tasks.

The history of planetary science may be said to have begun with the Ancient Greek philosopher Democritus, who is reported by Hippolytus as saying

The ordered worlds are boundless and differ in size, and that in some there is neither sun nor moon, but that in others, both are greater than with us, and yet with others more in number. And that the intervals between the ordered worlds are unequal, here more and there less, and that some increase, others flourish and others decay, and here they come into being and there they are eclipsed. But that they are destroyed by colliding with one another. And that some ordered worlds are bare of animals and plants and all water.[2]

In more modern times, planetary science began in astronomy, from studies of the unresolved planets. In this sense, the original planetary astronomer would be Galileo, who discovered the four largest moons of Jupiter, the mountains on the Moon, and first observed the rings of Saturn, all objects of intense later study. Galileo’s study of the lunar mountains in 1609 also began the study of extraterrestrial landscapes: his observation “that the Moon certainly does not possess a smooth and polished surface” suggested that it and other worlds might appear “just like the face of the Earth itself”.[3]

Advances in telescope construction and instrumental resolution gradually allowed increased identification of the atmospheric and surface details of the planets. The Moon was initially the most heavily studied, as it always exhibited details on its surface, due to its proximity to the Earth, and the technological improvements gradually produced more detailed lunar geological knowledge. In this scientific process, the main instruments were astronomical optical telescopes (and later radio telescopes) and finally robotic exploratory spacecraft.

The Solar System has now been relatively well-studied, and a good overall understanding of the formation and evolution of this planetary system exists. However, there are large numbers of unsolved questions,[4] and the rate of new discoveries is very high, partly due to the large number of interplanetary spacecraft currently exploring the Solar System.

This is both an observational and a theoretical science. Observational researchers are predominantly concerned with the study of the small bodies of the Solar System: those that are observed by telescopes, both optical and radio, so that characteristics of these bodies such as shape, spin, surface materials and weathering are determined, and the history of their formation and evolution can be understood.

Theoretical planetary astronomy is concerned with dynamics: the application of the principles of celestial mechanics to the Solar System and extrasolar planetary systems.

The best known research topics of planetary geology deal with the planetary bodies in the near vicinity of the Earth: the Moon, and the two neighbouring planets: Venus and Mars. Of these, the Moon was studied first, using methods developed earlier on the Earth.

Geomorphology studies the features on planetary surfaces and reconstructs the history of their formation, inferring the physical processes that acted on the surface. Planetary geomorphology includes the study of several classes of surface features:

The history of a planetary surface can be deciphered by mapping features from top to bottom according to their deposition sequence, as first determined on terrestrial strata by Nicolas Steno. For example, stratigraphic mapping prepared the Apollo astronauts for the field geology they would encounter on their lunar missions. Overlapping sequences were identified on images taken by the Lunar Orbiter program, and these were used to prepare a lunar stratigraphic column and geological map of the Moon.

One of the main problems when generating hypotheses on the formation and evolution of objects in the Solar System is the lack of samples that can be analysed in the laboratory, where a large suite of tools are available and the full body of knowledge derived from terrestrial geology can be brought to bear. Direct samples from the Moon, asteroids and Mars are present on Earth, removed from their parent bodies and delivered as meteorites. Some of these have suffered contamination from the oxidising effect of Earth’s atmosphere and the infiltration of the biosphere, but those meteorites collected in the last few decades from Antarctica are almost entirely pristine.

The different types of meteorites that originate from the asteroid belt cover almost all parts of the structure of differentiated bodies: meteorites even exist that come from the core-mantle boundary (pallasites). The combination of geochemistry and observational astronomy has also made it possible to trace the HED meteorites back to a specific asteroid in the main belt, 4 Vesta.

The comparatively few known Martian meteorites have provided insight into the geochemical composition of the Martian crust, although the unavoidable lack of information about their points of origin on the diverse Martian surface has meant that they do not provide more detailed constraints on theories of the evolution of the Martian lithosphere.[5] As of July 24, 2013 65 samples of Martian meteorites have been discovered on Earth. Many were found in either Antarctica or the Sahara Desert.

During the Apollo era, in the Apollo program, 384 kilograms of lunar samples were collected and transported to the Earth, and 3 Soviet Luna robots also delivered regolith samples from the Moon. These samples provide the most comprehensive record of the composition of any Solar System body beside the Earth. The numbers of lunar meteorites are growing quickly in the last few years [6] as ofApril 2008 there are 54 meteorites that have been officially classified as lunar.Eleven of these are from the US Antarctic meteorite collection, 6 are from the JapaneseAntarctic meteorite collection, and the other 37 are from hot desert localities in Africa,Australia, and the Middle East. The total mass of recognized lunar meteorites is close to50kg.

Space probes made it possible to collect data in not only the visible light region, but in other areas of the electromagnetic spectrum. The planets can be characterized by their force fields: gravity and their magnetic fields, which are studied through geophysics and space physics.

Measuring the changes in acceleration experienced by spacecraft as they orbit has allowed fine details of the gravity fields of the planets to be mapped. For example, in the 1970s, the gravity field disturbances above lunar maria were measured through lunar orbiters, which led to the discovery of concentrations of mass, mascons, beneath the Imbrium, Serenitatis, Crisium, Nectaris and Humorum basins.

If a planet’s magnetic field is sufficiently strong, its interaction with the solar wind forms a magnetosphere around a planet. Early space probes discovered the gross dimensions of the terrestrial magnetic field, which extends about 10 Earth radii towards the Sun. The solar wind, a stream of charged particles, streams out and around the terrestrial magnetic field, and continues behind the magnetic tail, hundreds of Earth radii downstream. Inside the magnetosphere, there are relatively dense regions of solar wind particles, the Van Allen radiation belts.

Geophysics includes seismology and tectonophysics, geophysical fluid dynamics, mineral physics, geodynamics, mathematical geophysics, and geophysical surveying.

Planetary geodesy, (also known as planetary geodetics) deals with the measurement and representation of the planets of the Solar System, their gravitational fields and geodynamic phenomena (polar motion in three-dimensional, time-varying space. The science of geodesy has elements of both astrophysics and planetary sciences. The shape of the Earth is to a large extent the result of its rotation, which causes its equatorial bulge, and the competition of geologic processes such as the collision of plates and of vulcanism, resisted by the Earth’s gravity field. These principles can be applied to the solid surface of Earth (orogeny; Few mountains are higher than 10km (6mi), few deep sea trenches deeper than that because quite simply, a mountain as tall as, for example, 15km (9mi), would develop so much pressure at its base, due to gravity, that the rock there would become plastic, and the mountain would slump back to a height of roughly 10km (6mi) in a geologically insignificant time. Some or all of these geologic principles can be applied to other planets besides Earth. For instance on Mars, whose surface gravity is much less, the largest volcano, Olympus Mons, is 27km (17mi) high at its peak, a height that could not be maintained on Earth. The Earth geoid is essentially the figure of the Earth abstracted from its topographic features. Therefore, the Mars geoid is essentially the figure of Mars abstracted from its topographic features. Surveying and mapping are two important fields of application of geodesy.

The atmosphere is an important transitional zone between the solid planetary surface and the higher rarefied ionizing and radiation belts. Not all planets have atmospheres: their existence depends on the mass of the planet, and the planet’s distance from the Sun too distant and frozen atmospheres occur. Besides the four gas giant planets, almost all of the terrestrial planets (Earth, Venus, and Mars) have significant atmospheres. Two moons have significant atmospheres: Saturn’s moon Titan and Neptune’s moon Triton. A tenuous atmosphere exists around Mercury.

The effects of the rotation rate of a planet about its axis can be seen in atmospheric streams and currents. Seen from space, these features show as bands and eddies in the cloud system, and are particularly visible on Jupiter and Saturn.

Planetary science frequently makes use of the method of comparison to give a greater understanding of the object of study. This can involve comparing the dense atmospheres of Earth and Saturn’s moon Titan, the evolution of outer Solar System objects at different distances from the Sun, or the geomorphology of the surfaces of the terrestrial planets, to give only a few examples.

The main comparison that can be made is to features on the Earth, as it is much more accessible and allows a much greater range of measurements to be made. Earth analogue studies are particularly common in planetary geology, geomorphology, and also in atmospheric science.

Smaller workshops and conferences on particular fields occur worldwide throughout the year.

This non-exhaustive list includes those institutions and universities with major groups of people working in planetary science. Alphabetical order is used.

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Planetary science – Wikipedia

Global Volcanism Program | Ambae

Caldera lake bubbling; burned vegetation

“Three anomalous ‘boiling’ areas with large bubbles and burned vegetation were observed at Lake Vui on 13 July, by P. Fogarty (Chief Pilot of VANAIR). This was the first time he had observed such a phenomenon, and he noted that the vegetation had still been green in May. An aerial survey of the two summit calderas was carried out (during a VANAIR flight) on 24 July. At that time, no strong degassing was visible, but 3 areas of discolored water (each several tens of meters in diameter) were noticeable in the crater lake. Burned vegetation was observed up to the crater rim, 120 m above the water. On 26 July, microseismicity in the caldera was very weak and without any volcanic characteristics.

“Although continuous weak solfataric activity occurs beneath Lake Vui (Warden, 1970), an anomalously strong SO2 degassing is believed to have occurred between May and July. This event was unnoticed by island residents, but since Aoba has been quiet for 300 years, vigilance for this kind of phenomenon must be improved. The existence of a summit caldera lake, numerous lahar deposits, and thick layers of ash (vesiculated and accretionary lapilli) demonstrate the hazards that would accompany renewed activity. Thus, as a precaution, a seismological station was installed in July on the SW flank of the volcano.

Reference. Warden, A.J., 1970, Evolution of Aoba caldera volcano, New Hebrides: BV, v. 34, p. 107-140.

Information Contacts: C. Robin and M. Monzier, ORSTOM, Nouma, New Caledonia; M. Lardy and C. Douglas, ORSTOM, Vanuatu; C. Mortimer, Dept. of Geology, Mines, and Rural Water Supply, Vanuatu; J. Eissen, ORSTOM, France.

Volcanic seismicity felt during 1-7 December

Unusual seismicity was felt by island residents during 1-7 December 1994, with a maximum of seven small-to-medium events on the 5th. These volcanic events were of high-frequency and lacked individualized phases. At the suggestion of ORSTOM, the National Disaster Management Office (NDO) organized a helicopter reconnaissance on 7 December to inspect the volcano for evidence of possible eruptive activity. Activity at the Lake Vui crater and the fumarolic area on the shore of Lake Manoro was similar to that observed during previous aerial observations on 24 July 1991 and September 1993. At Lake Voui, small areas of hot and gaseous water were evident and the rainforest was completely burned around the crater. No large bubbles like those noted on 13 July 1991 (10 m in diameter) were observed (BGVN 16:07). An automated seismic alert station, with satellite transmission to Port Vila, will be installed near Lake Voui.

Information Contacts: M. Monzier, ORSTOM and Vanuatu Department of Geology, Mines and Water Resources, Vanuatu.

Increased steam emissions and seismicity in early March; evacuation preparations made

The following report, prepared on 17 March, is from volcanologists of the Institut Francais de Recherch Scientifique pour le Developpement en Cooperation, Office de la Recherch Scientifique et Technique Outre-Mer (ORSTOM), in Vanuatu and Ecuador.

Geological setting. Aoba is the largest basaltic shield volcano in the New Hebrides arc, with the base ~3,000 m below sea level, the summit ~1,500 m asl, and a volume of ~2,500 km3 (Eggins, 1993; Gorton, 1977; Robin and others, 1993). This rainforest-covered island lies in front of the d’Entrecasteaux collision zone, between the N and S Aoba Basins along an ~N50E fracture transverse to the arc (figure 1; see Greene and others, 1994, for more information). Two concentric summit calderas, the largest 5 km in diameter (figure 2), enclose the central crater containing the 2-km-diameter Lake Voui (Vui) (figure 3). Numerous secondary craters and cones lie along the N50E fracture, out to the extremities of the island, where previous magma-seawater interactions have produced several maars.

Eruptive history. Lake Voui and the Manaro Ngoro summit explosion craters and cones formed ~420 years ago. The Ndui Ndui lava flows issued from the N50E fissure ~300 years ago and reached the NW coast (Warden, 1970). Possible eruption-related lahars (or only secondary mudflows following heavy rains?) annihilated villages on the SE flanks of the island ~120 years ago, producing several casualties. An eruption possibly occurred in 1914 with ashfalls (?) and lahars (12 casualties). . . .

Robin and Monzier (1993, 1994) consider Aoba the most potentially dangerous volcano of the Vanuatu archipelago because of the wide distribution of very young deposits related to strong explosive eruptions. They also cite thick lahar deposits, the presence of Lake Voui, long repose periods (~300-400 years , Warden, 1970), strong degassing at the lake in 1991, and a population of ~3,500 within 10 km of the crater.

Activity in December 1994. Unusual seismicity was felt . . . during 1-7 December 1994 (BGVN 20:01). Records from ORSTOM seismic stations on Santo (70 km W) and Efate (260 km SSE) islands showed that peak activity lasted 24 hours with 13 events, the largest M 4.6 (Regnier, 1995). Crustal hypocenters were located under the S submarine base of the volcano. On 7 December, helicopter reconnaissance showed small areas of rising hot gaseous water at Lake Voui, similar to July 1991 and September 1993, but the rainforest appeared completely burned for up to several hundred meters around the crater. Despite the end of the seismic crisis, ORSTOM emphasized to the NDO the need to remain circumspect of the volcano. In mid-December, according to Robin and Monzier (1994), the following advice was given to NDO: “In the case of a resumption of volcanic activity in the summit area, it will be wise to evacuate, in a first phase, the population of coastal villages of the central part of the island (in a 10 km radius area surrounding Lake Voui) towards the less hazardous NE and SW extremities of the island. If the eruption occurs near these extremities, or spreads along fractures from central vents towards these extremities, then it might be necessary to evacuate part of the population to Santo or Maewo-Pentecost.”

Activity in March 1995. According to a VANAIR pilot report on 1 March, Lake Voui was calm with gas emissions from numerous locations. The following day, the lake was steaming all over, bubbling up in the center, and its surface was rough; the pilot also reported black sediment ejections. Early on the morning of 3 March, people on Santo Island observed a gas plume rising 2-3 km above Lake Voui. Simultaneously, crustal seismicity similar to that in December 1994 was recorded.

On 4-6 March, ORSTOM geophysicists (M. Lardy and D. Charley) recorded strong continuous tremor at Ndui Ndui, ~9 km NW from the main crater. This tremor had a monochromatic signal with a 1.4 Hz mean frequency, several hours duration, and an amplitude of 3-4x background. Local observers were trained to watch the activity and the collaboration with VANAIR pilots was reinforced. As usual during the tropical summer, the top of the volcano was covered by thick clouds and rarely visible. However, on 5 March a gas plume was still visible above Lake Voui.

An island resident who stayed several days in the summit area during early March described lake levels and reported that soft mud had been blown all over the shores. On 4 and 6 March the surface of Lake Voui was at least 5.4 m higher than normal. However, on 9 March the lake was hot and steaming, and was ~4.8 m below the normal level, a change of ~10 m within 3 days. Tremor activity remained constant between 9 and 13 March, but with significantly less intensity than during 4-6 March. In addition, shallow, local micro-seismicity was noted since 11 March. During an aerial survey on 13 March, the entire lake was steaming and a strong sulfur smell had been reported around the summit area.

If activity increases in the central crater, magma-water interactions could produce falls of ash, dense lapilli, and accretionary lapilli, as well as pyroclastic flows, base surges and lahars. Lava flows may also erupt from flank fissures, N50E or other orientations. The ORSTOM seismological team in Vanuatu will be reinforced on 17 March by the arrival of a new seismologist, and 5-7 portable seismic stations will be deployed around the island as soon as possible to improve the focal locations and delineate possible areas of attenuation. Also, a new permanent seismic station will be installed on Aoba. Daily contact is maintained between ORSTOM scientists in Vanuatu and Ecuador; the latter are prepared to move to Vanuatu if necessary.

Evacuation preparations. On 8 March, after discussions between ORSTOM geophysicists in Vanuatu and volcanologists now based in Ecuador, the following advice was given to the Vanuatu Government: “. . .The size of the gas plume observed above Lake Voui crater on March 3, 1995 probably means that magma is now rising within the volcano . . . . Thus, Aoba volcano is now dangerous and it seems necessary to envisage the evacuation of the population of coastal villages located in a 10 km radius area surrounding Lake Voui towards the less hazardous NE and SW extremities of the island . . . .”

Following this advice, Aoba Island was placed on alert and preparations for evacuations were begun. On 9 March, aircraft within a 4-km radius of Aoba up to 2.2 km altitude (7,500 feet) were restricted to scheduled flights and those approved by civil aviation or disaster office authorities. Correcting previous statements that evacuations had already started, the UNDHA reported on 17 March that villages within 10 km of the crater had been identified as threatened, and those within a 5-km radius had been placed on stand-by for immediate evacuation. Evacuation centers were identified, and all available government and several private ships were positioned to assist in a possible evacuation.

References. Eggins, S., 1993, Origin and differenciation of picritic arc magmas, Ambae (Aoba), Vanuatu: Contributions to Mineralogy and Petrology, v. 114, p. 79-100.

Gorton, M.P., 1977, The geochemistry and origin of quaternary volcanism in the New Hebrides: Geochimica et Cosmochimica Acta, v. 41, p. 1257-1270.

Greene, H.G., Collot, J.-Y., Stokking, L.B., and others, 1994, Proceedings of the Ocean Drilling Program, Scientific Results, 134: College Station, TX (Ocean Drilling Program).

Regnier, M., 1995, Rapport prliminaire sur la crise sismique d’Aoba de dcembre 1994: Rapport ORSTOM, Port-Vila, 4 p.

Robin, C., and Monzier, M., 1993, Volcanic hazards in Vanuatu: Disaster Management Workshop by National Disaster Management Office, Republic of Vanuatu, 24-28 May 1993, Port-Vila, 8 p.

Robin, C., and Monzier, M., 1994, Volcanic hazards in Vanuatu: ORSTOM and Dept. of Geology, Mines and Water Resources of the Vanuatu Government report, 15 p.

Robin, C., Monzier, M., Crawford, A.J., and Eggins, S.M., 1993, The geology, volcanology, petrology-geochemistry, and tectonic evolution of the New Hbrides island arc, Vanuatu: IAVCEI Canberra 1993, Excursion guide, Record 1993 / 59, Australian Geological Survey Organisation, 86 p.

Warden, A.J., 1970, Evolution of Aoba caldera volcano, New Hebrides: BV, v. 34, no. 1, p. 107-140.

Information Contacts: C. Robin and M. Monzier (geologists) ORSTOM, Quito, Ecuador; M. Lardy (geophysicist); M. Regnier, J-P. Metaxian, R. Decourt (seismologists), and D. Charley (technical assistant), ORSTOM, Vanuatu; M. Ruiz (seismologist), Instituto Geofsico, Escuela Politcnica Nacional, Quito, Ecuador; J-P. Eissen (geologist), ORSTOM, France; BOM, Australia; UNDHA.

Crater lake exhibits convection cells and steaming as level drops

A pyroclastic explosion on the morning of 3 March 1995 generated a vapor-and-ash column ~3 km high (BGVN 20:02). Preliminary analysis of the resulting deposit did not reveal any juvenile material. On the morning of 5 March, a vapor plume rose ~500 m. It is possible that vapor plumes were emitted over several days, but were not observed at other times because of the thick clouds that usually hide the summit area. The center of activity on 3 March was between two small islands in Lake Voui (figures 4 and 5). Because of poor weather conditions, ORSTOM scientists were unable to observe the lake at close range until 13 March. Aerial photos taken on 20 March (figure 6) show the thermal contrast between Lake Manaro Lakua, formed by the accumulation of water in a low-lying area of the caldera, and Lake Voui, which fills the active crater. Convection cells, ~300-400 m in diameter, could be discerned within Lake Voui.

A drop in the level of Lake Voui that began on 6 March (BGVN 20:02) was visible in photographs taken on 20 March. During another overflight on 6 April, the level of the crater lake had dropped by ~2 m. By the time of a 27 June landing on the NW island in Lake Voui (figure 5), the lake level had dropped ~5 m below the maximum, as determined by recent vegetation. Water temperatures measured around the most accessible parts of the island averaged 38-40C, with highs of 63-67C. The strongly acidic (pH 2.3) emerald-green lake was mostly obscured by clouds, but vapor emissions were visible between the island and the NW edge of the crater. A small island seen on 6 April in the N part of the lake had enlarged noticeably because of the drop in water level. The topography of the islands is steep towards the center of the lake and gentle towards crater edge. All of the trees on the island were dead, but other vegetation was beginning to reappear. Some blocks of dried mud (40-50 cm in diameter) ejected during the phreatic explosion at the beginning of March were still visible. Sulfur deposits were noted, and gas bubbles were coming from numerous fissures at the edge of the island.

A bathymetric survey of Lake Voui has never been done, but ORSTOM estimates that it has a volume of 50 million cubic meters. Although activity has declined in recent months, ORSTOM will maintain the current low-level alert status until approximately the end of November.

Information Contacts: M. Lardy, D. Douglas, P. Wiart, and K. Kalkaua, Centre ORSTOM, Port Vila, Vanuatu, and Bureau des Desastres Nationaux, P.M.B. 014, Port Vila, Vanuatu; M. Regnier and S. Temakon, ORSTOM et Departement des Mines et de la Geologie et des Ressources en Eaux, Port Vila, Vanuatu; Chief N. Tahi, Village de Nambangahake (Ndui-Ndui) Aoba, Vanuatu; C. Robin and M. Monzier, Centre ORSTOM, Quito, EcuadorJ-P.Eissen, Centre ORSTOM de Brest, France; J-P. Metaxian, Universite de Savoie.

Monitoring and water chemistry at Voui crater lake

Following the 1995 phreatic explosion at Lake Voui (BGVN 20:02 and 20:08) a bathymetric survey of the crater lake was carried out. The 1996 survey confirmed the location of activity that had first been observed in 1992 on a SPOT satellite image. Monitoring of Lake Voui has continued through November 1998.

The average temperature over the whole 1 x 2 km surface of the lake (figures 7 and 8) stayed at ~30C during November 1996-November 1998, due in part to constant streams of gas that issued from the main vent. As a comparison, in June 1995, three months after the phreatic explosion, the surface temperature was 45C.

The ten major compounds dissolved in the lake’s water have changed in concentration with time (table 1), but the samples, taken at the surface and at depths of 15-50 m, were consistent throughout the lake at any one time.

Table 1. Synopsis of the physical and chemical analysis of the waters of Voui lake derived from samples taken during 1995-98. Chemical constituents and ratios are given in mg/L. Courtesy Centre ORSTOM, Vanuatu.

The average volume of the lake was estimated at 50 x 106 m3, but the level varied significantly. A drop of 275 cm in surface elevation was observed between June 1997 and October 1998. Rainfall varied between 500 and 600 cm/year in the summit area.

Monitoring was conducted twice per year, complemented by seismic recordings taken from a station set up in the dry lake bed of Ngoro. This system is similar to that used on Tanna Island, Vanuatu (BGVN 21:08). The range of monitoring equipment in place on Aoba since 1996 was extended in October 1998 by the installation of an acoustic recording station (0.1-150 KHz) and a device for continuous measurement of lake-water temperature. The data are relayed through an ARGOS satellite transmitter. Identical stations have been set up on Kelut in Indonesia and at Lake Taal in the Philippines.

Information Contacts: Michel Lardy, Ins Rodriguez, Douglas Charley, and Pascal Gineste, Centre ORSTOM, P.O.Box 76, Port-Vila, Vanuatu; Michel Halbwachs, and Jacques Grangeon, Universit de Savoie, Campus Scientifique, F3376, Le Bourget du Lac, Cdex France; Janette Tabbagh, Centre de Tlobservation Informatise des volcans, CNRS-CRG, Garchy, France.

Increase in temperature and acidity at Lake Voui during April-August 2000

Since phreatic eruptions occurred at Voui crater lake in March 1995 (BGVN 20:02 and 20:08) the lake has been closely monitored. No reports of activity were received after October 1998 (BGVN 23:10) until Lake Voui’s temperature and acidity increased above normal levels during April through August 2000. Charlie Douglas and Sandrine Wallez reported that in mid-April 2000 the temperature at Lake Voui was ~27C, but by August it had increased to 35.8 C (figure 9), which was the highest temperature recorded since they began monitoring the lake in 1998. They also reported that the water’s acidity increased. Water analysis conducted on 15 June indicated that the increases were the result of an injection of fumarolic gases into the lake, perhaps related to ascent of new magma.

Information Contacts: Stromboli On-line, maintained by Jrg Alean and Roberto Carniel (URL: http://www.swisseduc.ch/stromboli/); Charlie Douglas and Sandrine Wallez, Geohazard Mitigation Section, Department of Geology, Mines, and Water Resources of Vanuatu (URL: http://www.sidsnet.org/pacific/sopac/members/vu.html); Michel Lardy and Michel Halbwachs, Institut de recherche pour le dveloppement (IRD), P.O. Box 76, Port Vila, Vanuatu.

Sustained elevation of Lake Voui’s temperature indicates increased heat transfer

Voui crater lake’s temperature and hydro-acoustic signals are measured continuously by an automated station that transmits in real time via satellite (BGVN 23:10). Recent measurements revealed heavy activity under the lake during March-June 2000 (BGVN 25:08), when the estimated 50 x 106 m3 volume of water rapidly increased in temperature by more than 7C (figure 10).

The increase was accompanied by acoustic signals covering a wide range of frequencies (figure 10, bottom). Those in the audible band (> 100 Hz) were thought to be associated with the emission of gas bubbles and an increase in submarine fumarolic activity. Those in the ultrasound band (30-190 kHz) could stem from fluids circulating within the hydrothermal zone beneath the lake (figure 11).

A consistent first-order rise in water temperatures persisted through December 2000 (figure 12). Despite seasonal variations in air temperature and the cooling effect of heavy tropical rainfall (~5 m/yr), Lake Voui’s temperature remained stable at ~36C as of January 2001. The preceding rise and sustained high temperature indicate continued heat transfer from the bottom of the lake. The effect appears more substantial than the heating seen between 1996 and 1999, when water temperature averaged ~30C.

Information Contacts: Michel Lardy, Institut de Recherche pour le Dveloppement (IRD), Centre d”Ile de France 93143 Bondy Cdex, France; Michel Halbwachs, Universit de Savoie, BP1104, F 73376 Le Bourget du Lac Cdex, France; Jeanne Tabbagh, Universit Pierre et Marie Curie, Dpartment de gophysique applique, 75252 Paris Cdex O5, France; Douglas Charley, Department of Geology, Mines, and Water Resources, PMB01, Port-Vila, Vanuatu, Oceania.

New eruption begins on 27 November 2005 and builds cone in crater lake

A new eruption began on 27 November 2005 when vapor plumes and ash columns were observed originating from Lake Voui, a crater lake at the summit of Aoba (figure 13). The volcano is also referred to locally as Manaro or Lombenben. Prior to this activity, the most recent reported volcanism consisted of phreatic explosions from the lake during March 1995 (BGVN 20:01, 20:02, and 20:08). Bathymetry conducted by ORSTOM in 1996 showed that the vent feeding gases and magma into Lake Voui had a depth of about 150 m and a diameter of about 50 m. The volume of water in the lake (1 x 2 km) totals some 40 million cubic meters, with a mean pH of 1.8. Lake Voui and the Manaro Ngoro summit explosion craters and cones formed ~ 420 years ago (figure 14). Lake Manaro was formed by the accumulation of water in a low-lying area of the Manaro summit caldera.

Starting on 3 December a team of volcanologists from the Vanuatu Department of Geology, Mines, and Water Resources (DGMWR), the French Institut de recherche pour le dveloppement (IRD), the New Zealand Institute of Geological & Nuclear Sciences (GNS), and New Zealand’s Massey University began collaborating on observations and monitoring. The amplitude of tremor recorded by DGMWR instruments from 30 November to 3 December was lower than during the March 1995 activity.

Scientists who visited the lake on 4 and 5 December (figures 15 and 16) observed a similar style of eruptive activity on both days, but some individual explosions appeared larger on the 5th. It was not possible to reach the lake to collect a water sample. There appeared to be two active vents, side by side, in the lake. One was producing eruptions of mud, rocks, and water, and the other appeared to be the source of the large continuous steam plume rising above the crater; the plume did not contain ash. There were no reports of ash falling on the island since the start of the eruptions the previous week. The team estimated that the cone being built in the lake, at an estimated height of more than 20 m on the 4th, was about 70% complete around the active vents, and grew 5-10% higher between 4 and 5 December. Continuous tremor was recorded during this time, and the level of eruptive and seismic activity seemed to be fairly stable.

Cloud cover and rain prevented a visit to the lake on 6 and 7 December. Earthquake recorders from the GNS were installed at the Provincial Centre at Saratamata, the Longana Peoples Centre (Lovonda village), and at Tahamamavi (“place of warm sea”) (figure 17). On 7 December, a final recorder from the IRD was installed near Nduidui on the SW side of the island. Over 6-7 December continuous moderate-level volcanic tremor was recorded, with no significant change in its level; there was no other significant seismic activity.

On 8 December, the group noted that small-scale eruptions continued in Lake Voui, building a volcanic cone in the lake and producing a tall (2.4-3.0 km) steam-and-gas plume. Afternoon observations showed the cone growing taller and surrounding three sides of the active vents. However, the cone was not complete on its E side, allowing lake water to react with the rising magma. Though the resulting explosions became further apart and slightly larger, the total energy involved appeared similar to 4-5 December. There continued to be two active vents, one producing the small explosions, and the second the steam and gas emissions. Seismic recorders continued to record volcanic tremor, but very few local earthquakes. No volcanic ash was present in the plume. The eruption had no immediate effect beyond Lake Voui. The Volcanic Alert Level remained at Level 2. The level of seismic activity seemed to be stable. No other significant seismic activity was recorded.

While departing by air on the evening of 8 December, the group clearly saw the active vents (figure 18). The cone had grown to the W, joining and partly burying one of the old islands. All eruptions occurred from inside the cone. The largest individual eruptions threw material 150-200 m above the lake. There was also a gas-and-steam vent present within the cone, W of the other vent. The level of the lake appeared unchanged.

On 10 December, the small-scale volcanic eruption continued from active vents within the summit crater lake (Lake Voui). Molten material entered the crater lake and reacted with the water to produce small explosive eruptions and a plume of steam and gas. The eruption built a cone around the active vents, enclosing them on three sides, forming an island about 200 m across and 50-60 m high. There were two vents, one erupting water, rocks and mud, and the other producing a tall column of steam and gas. The eruption had little effect outside the crater lake (minor ashfall occurred only in the first three days of the eruption). Five days of seismic recordings show a moderate level of seismic activity (mostly volcanic tremor).No change was noted in the level of Lake Voui, and there was also no evidence of ground uplift or fractures near the lake.

Sulfur dioxide measurements. SO2 data collected using a DOAS spectrometer on the Islander planes of Unity Air Lines (3 December) and Air Vanuatu (5 December). On 3 December the flux was 32.6-33.6 kg/s (~ 2,900 metric tons/day). By 5 December the flux had decreased about 25%, to 24.7-26.4 kg/s (~ 2,300 metric tons/day). SO2 was clearly detected by the OMI (ozone monitoring instrument) sensor on the NASA Aura satellite (figure 19). One measurement of the volcanic gas output on 10 December showed a moderate level of sulfur dioxide (SO2) gas (about 2,000 t/d) from the active vents.

Lake temperatures. A monitoring station for continuous measurements of water temperature at Lake Voui was installed in October 1998. The station used a satellite ARGOS transmission system and recorded the last heating episode of 2001 (figure 20), but failed after three years due to the harsh acid environment. ASTER thermal infrared images can also be used for monitoring lake surface temperatures, and Aoba has a freshwater lake (Manaro Lakua) which can be used to remove the seasonal/diurnal variations in atmospheric temperatures. Unfortunately, the top of the volcano is frequently covered by clouds and few ASTER images are exploitable. The most recent ASTER image clearly showing both lakes was collected on 9 July 2005. Difference in temperatures between lake Voui and Lakua was 4.0C, slightly above background values during 2002-2003. Maximum background temperatures measured with ASTER during the September 2002-October 2005 were at 26.3C. The last ASTER images before the eruption, on 5 October 2005, showed no unusual temperatures at Lake Voui.

MODIS satellites have a more frequent coverage than ASTER but their spatial resolution is only 1 km. The surface area of Lake Voui (2.1 km2) is too small for an accurate measurement of lake temperature, but MODIS can detect rough temperature changes or an increased thermal anomaly. The MODIS pixel footprint is about 1 km along track and 2 km across track, so the measured temperatures are a mixed signal corresponding to the lake and some signal from the adjacent tropical forest (much colder than the lake at night at this elevation). MODIS SST imagery showed a strong thermal anomaly on 21 November 2005 (figure 20). Approximate lake temperatures, likely a minimum, were 30.4C on 20 November and 29.5C (Terra)/ 31.4C (Aqua) on 21 November. On 25 November the temperature jumped to about 42C.

Reference. Cronin, S.J., Gaylord, D.R., Charley, D., Alloway, B.V., Wallez, S., and Esau, J.W., 2004, Participatory methods of incorporating scientific with traditional knowledge for volcanic hazard management on Ambae Island, Vanuatu: Bulletin of Volcanology, v. 66, p. 652-668. (URL: http://www.proventionconsortium.org/files/tools_CRA/CS/Vanuatu.pdf)

Information Contacts: Esline Garaebiti, Douglas Charley, Morris Harrison, and Sandrine Wallez, Department of Geology, Mines, and Water Resources (DGMWR), Port-Vila, Vanuatu; Michel Lardy, Philipson Bani, Jean-Lambert Join, and Claude Robin, Institut de recherche pour le dveloppement (IRD), BP A5, 98 848 Nouma CEDEX, New Caledonia (URL: http://www.suds-en-ligne.ird.fr/fr/volcan/vanu_eng/aoba1.htm); Brad Scott and Steve Sherburn, Institute of Geological & Nuclear Sciences (GNS), Wairakei Research Center, Taupo, New Zealand; Shane Cronin, Institute of Natural Resources, Massey University, Palmerston, New Zealand; Alain Bernard, IAVCEI Commission on Volcanic Lakes, Universit Libre de Bruxelles, Brussels, Belgium (URL: http://www.ulb.ac.be/sciences/cvl/aoba/Ambae1.html); NASA Earth Observatory (URL: http://earthobservatory.nasa.gov/); United Nations, Office for the Coordination of Humanitarian Affairs (OCHA), Regional Office for Asia and the Pacific.

Landscape changes resulting from November 2005 eruption

As previously reported (BGVN 30:11), a new eruption of Aoba began on 27 November 2005 when vapor plumes and ash columns were observed originating from Lake Voui, a crater lake at the summit. Activity continued into early January, building a large cinder cone in the west-central part of Lake Voui (figure 21). The new cone also contained its own crater lake.

An image taken by ASTER’s visible, near infra-red (VNIR) telescope on 24 December 2005 (UTC) showed the two larger caldera lakes, and steam escaping from an island in the center of Lake Voui (figure 22). The VNIR telescope has a resolution of ~ 15 m and operates in the spectral range 0.52-0.86 ?m.

During September through December 2005, infrared satellite data provided by Moderate Resolution Imaging Spectroradiometer (MODIS) and processed by the MODVOLC Hot-Spot algorithm at the Hawaii Institute of Geophysics and Planetology (HIGP) only observed a single-pixel thermal anomaly. It occurred at 0110 local time on 26 November 2005 ( the image was acquired at 1410 UTC on 25 November 2005). That was 1 day prior to reports of the eruption from ground-based observers, although the ground-based reports could easily have been delayed so it is not clear that the MODVOLC thermal anomaly was actually prior to ground based observations.

Matt Patrick noted that the anomaly is nicely centered in the caldera and is almost certainly volcanic ? no other anomalies occurred on the island in the previous 5 years.

Information Contacts: Alain Bernard, IAVCEI Commission on Volcanic Lakes, Universit Libre de Bruxelles, Brussels, Belgium (URL: http://www.ulb.ac.be/sciences/cvl/aoba/Ambae1.html); NASA Earth Observatory (URL: http://earthobservatory.nasa.gov/); Esline Garaebiti, Department of Geology, Mines and Water Resources, Port Vila, Vanuatu; Matt Patrick, University of Hawaii, Hawaii Institute of Geophysics and Planetology (HIGP) Thermal Alerts Team, 2525 Correa Road, Honolulu, HI 96822 (URL: http://modis.higp.hawaii.edu/).

Crater-lake photos and satellite temperatures data show ongoing activity

As previously reported, a new eruption at Aoba began 27 November 2005 in one of the crater lakes (Lake Voui). The eruption formed a cinder cone in the lake (figures 23 and 24) that contained a crater with a small hot lake (BGVN 30:11 and 30:12).

On 31 January a high, dark ash plume caused ashfall in the S part of the island. Small eruptions continued in February.

Alain Bernard recently processed a 26 January 2006 nighttime ASTER (Advanced Spaceborne Thermal Emission and Reflection Radiometer) image. Figure 25 shows the ASTER product called AST_04 (TIR?thermal infrared radiometer, 8.12-11.65 ?m wavelengths?band 10) unprocessed image of Aoba with Lakes Voui and Lakua. The TIR bands, with a spatial resolution of 90 m, give the ability to detect small thermal anomalies (a few degrees C), perform thermal mapping, and monitor temporal variations in the lake surface temperature. As shown in figure 26, Lake Voui’s temperature in early January 2006 dropped by ~ 10C to a mean of 25.4C (down from 35.7C one month earlier). Temperature differences between Voui and Lakua dropped to 4.3C, reaching almost to the background levels observed in July 2005 (see plot “Temperature data from Lake Voui at Aoba, October 1998-December 2005 . . .”; BGVN 30:11). There is still a strong thermal anomaly of 46.1C inside the new island (figure 13).

As of 11 February 2006 at 1011 hours (10 February 2006 at 2311 UTC), Alain Bernard reported that Lakes Voui and Lakua temperatures were, respectively, 27.2C and 23.2C (delta T = 4C). The maximum temperature for the mud pool was ~ 57C.

Information Contacts: Alain Bernard, IAVCEI Commission on Volcanic Lakes, Universit Libre de Bruxelles (ULB), CP160/02, avenue F.D. Roosevelt 50, Brussels, Belgium (URL: http://www.ulb.ac.be/sciences/cvl/aoba/Ambae1.html, http://www.ulb.ac.be/sciences/cvl/multispectral/multispectral2.htm); Esline Garaebiti, Department of Geology, Mines, and Water Resources (DGMWR), Port-Vila, Vanuatu.

During May-June 2006, Lake Voui’s water rapidly turns from blue to red

Alain Bernard reported that Lake Voui in Aoba-Ambae volcano (BGVN 31:01) was undergoing a spectacular change in its color?the previously aqua-colored lake was turning red (figure 27).

Images of a pale reddish Lake Voui were obtained by Esline Garaebiti, who flew over the volcano 28 May 2006. Philippe Mtois, who flew over on 3 June 2006, photographed a blood-red lake. These photos were are posted on the CVL website along with recent ASTER temperature data. This color change was tentatively attributed to a rapid shift in the lake water’s redox state. The change might be linked to the ratio of SO2/H2S in the hydrothermal fluids.

Information Contacts: Alain Bernard, IAVCEI Commission on Volcanic Lakes (CVL), Universit Libre de Bruxelles (ULB), CP160/02, avenue F.D. Roosevelt 50, Brussels, Belgium (URL: http://www.ulb.ac.be/sciences/cvl/aoba/Ambae1.html, http://www.ulb.ac.be/sciences/cvl/multispectral/multispectral2.htm); Esline Garaebiti, Department of Geology, Mines, and Water Resources (DGMWR), Port-Vila, Vanuatu; Philippe Mtois, World of Wonders.

Acidic gas emissions destroy vegetation; islet lake breached

The Aura/OMI satellite detected elevated SO2 concentrations above Aoba volcano during July and August 2006. Comparison of MODIS imagery between 3 June and 31 August 2006 (figure 28) revealed the effects of emissions on vegetation around the crater. The conditions in the field were investigated by a scientific team from Institut de Recherche pour le Dveloppement (IRD). They concluded that a significant area of the summit (30 to 40 km2) was burned by acid gas emissions.

When IRD scientists conducted a visit to Aoba in late November 2006 vegetation surrounding the crater lake had been recently defoliated (figure 29), with trees completely burned and dead, due to plumes of acidic gas and aerosols during June-August 2006. They also concluded that heavy rainfalls since September 2006 diluted the acidity of plumes. Occasional green spots seen during the November visit were where new growths of ferns and tree ferns had become established. The acid effects were more extensive than previously seen since the early 1990s. This new behavior may reflect increased degassing from the source vent inside the ring-shaped tephra (or tuff) cone.

On 25 November 2006 an IRD team measured an SO2 flux of 3,000 tons/day. This value coincided with the measurement provided by the ozone monitoring instrument (OMI on the EOS Aura satellite). The value represented a marked reduction in SO2 degassing compared to that measured on 10 June 2006.

The team noted that the main lake in the crater, Lake Voui, was still a red color, an effect due to oxidation of the iron in its large mass of water (BGVN 31:05). Within that larger lake resides the ring-shaped island, which largely formed during the late 2005-early 2006 eruptions (BGVN 31:01). The island’s form had been that of an unbroken ring, but by the time of their 25 November visit, the preceding month’s heavy rains had eroded the smaller islands wall, allowing water in the two lakes to easily mix (figure 30). The W shore of Lake Voui has also been eroded, and fumaroles were observed in the lake. The breach in the tephra ring coincided with gas emissions ceasing.

The IRD team implemented the first permanent real-time temperature monitoring during their visit. Due to the heavy rainfall since June 2006 and the lowered levels of evaporation associated with the lowered average lake temperature (~ 25C on 25 November 2006), the lake level remained high. In addition, the average level of Lake Voui is higher due to volcanic material (ash, scoria) deposited between December 2005 and January 2006, and it should continue to fluctuate seasonally, as in the past.

Information Contacts: Michel Lardy, Institut de Recherche pour le Dveloppement (IRD), BP A 5 98 848 Noumea Cedex, New Caledonia (URL: http://nouvelle-caledonie.ird.fr/); Department Geology Mines and Water Resources (DGMWR), Geohazard Section, PMB 01 Port-Vila, Republic of Vanuatu; Alain Bernard, Universite Libre de Bruxelles, Brussels, Belgium (URL: http://www.ulb.ac.be/sciences/cvl/aoba/Ambae1.html).

Increased degassing starting December 2009

Our last Bulletin report (BGVN 31:12) on Aoba (Ambae) described the destruction of vegetation by acidic gas emissions and the breach of the islet lake during 2006. This report discusses comparative quiescence into late 2009 when degassing escalated (substantial gas plumes were seen) and the hazard status rose. The volcano has remained quiet into mid-2011.

The Vanuatu region lies ~2,200 km N off the New Zealand coast and ~2,100 km NE off the coast of Australia (figure 31). A 1999 census suggested ~9,400 people resided on Ambae. Cronin and others (2004) describe the residents as “dispersed amongst more than 276 small extended family settlements and villages (Wallez 2000). Settlements are mostly restricted to the lower island slopes within 4 km of the coast. The highest population densities occur at the NE and SE ends of the island.”

The Vanuatu Geohazards Observatory (VGO) noted increases in activity from Aoba (Ambae) starting in December 2009.This began when local villagers near the volcano reported seeing a plume over the island. In December 2009 the Vanuatu Volcanic Alert Level (VVAL) was raised to Level 1. The scale ranges from 0 to 4: 0 represents normal low-level activity and 4 represents a large eruption and island wide danger. The reported source of activity is a recent cone located in the crater lake, Voui (BGVN 30:11 and 30:12).

The VGO went on to note that “An expatriate pilot based on Gaua, also witnessed a plume on Ambae on Tuesday 6th April on his way back to Gaua from Santo. Aerial pictures that were taken by two Geohazards staff on 11 April 2010 also confirmed gas emissions that were more concentrated than normal… [which] reaffirms the [Ozone Monitoring Instrument or OMI] satellite image of gas emissions above. Another observation made on Ambae is the presence of sulphur-hydromagmatic activity on the SE part of the second crater of Ambae enclosing Manaro Lakua indicated by what seemed like two fumarolic zones…. There was also some discoloration of the water in Manaro Lakua near the ‘fumaroles’ with some areas near the shore [colored] brown, and some areas [colored] pale bluea sign of the incorporation of sulphur dioxide. It was also reported that while flying above the area, strong sulphur dioxide gas could be smelt even at 5,000 feet [~1.5 km altitude] on 11 April.”

The VGO also noted that the OMI satellite pictures depicted fluctuating gas emissions during this period. The image for 11 April 2010 indicated elevated SO2 and gave the integrated concentration-pathlength as 15 kilotons. On this day, VGO had noted SO2 fluxes over 3,000 tons/day.

References. Cronin, SJ, Gaylord, DR, Charley, D., Alloway, BV, Wallez, S, and Esau, JW, 2004, Participatory methods of incorporating scientific with traditional knowledge for volcanic hazard management on Ambae Island, Vanuatu, Bulletin of Volcanology, v. 66, pp.652-668, Springer-Verlag.

Wallez S, 2000, Socio-economic survey of the impact of the volcanic hazards for Ambae Island: geo-hazards mitigation program section. Department of Geology, Mines and Water Resources, Port Vila, Vanuatu. p 39.

Information Contacts: Vanuatu Geohazards Observatory (VGO) (URL: http://www.vmgd.gov.vu/vmgd/); Ozone Monitoring Instrument (OMI), Sulfur Dioxide Group), Joint Center for Earth Systems Technology, University of Maryland Baltimore County (UMBC), 1000 Hilltop Circle, Baltimore, MD 21250, USA (URL: https://so2.gsfc.nasa.gov/).

Minor activity likely continuing into early 2013

In our May 2011 Bulletin we reported that there was increased degassing at Aoba (also known as Ambae) starting December 2009 through at least April 2010. This report summarizes notices pereiodically posted by the Vanuatu Geohazards Observatory (VGO) and covers the time interval from 4 June 2011 through 26 February 2013. The Vanautu Volcano Alert Level (VVAL) remained at 1 (on a scale of 0-4.)

Observations on 4 June 2011 revealed that small explosions had been occurring from the crater lake and were accompanied by local ashfall around the crater. Some villagers in the N and W parts of the island had observed the explosions.

Based on analysis of data collected by the Vanuatu Meteorology and Geohazards Department (VMGD), the Vanuatu Geohazards Observatory reported that a small series of explosions from Aoba occurred on 10 July 2011. On July 11, VGO noted that there had been recent increases in activity from Ambae and that local earthquakes were volcanic. Satellite images collected by the Ozone Monitoring Instrument showed sulfur dioxide emissions. Photos showed that the volcano was quiet on 12 July 2011, although ongoing earthquakes were detected.

According to the VGO, Ambanga villagers reported that minor activity at Aoba began in December 2012. The OMI instrument detected strong gas emissions on 18 and 25 January 2013; the emissions continued at a lower level through 7 February. Field observations by the Geohazards team during 30 January-2 February 2013 confirmed that activity had significantly changed. Data retrieved from a monitoring station also confirmed ongoing activity. Satellite images acquired on 3 and 26 February 2013 detected substantial sulfur dioxide emissions.

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Global Volcanism Program | Ambae

palus – Wiktionary

English[edit]Etymology 1[edit]

From Latin plus (stake, post). Doublet of pole.

palus (plural pali)

From Latin pals (marsh, swamp).

palus (plural paludes)

palus?

From Proto-Italic *palts, *pald-, from Proto-Indo-European *pelHk-iH-h, related to Latvian pelce (puddle), Lithuanian pelk (marsh), Sanskrit (palvala, pool, pond), and possibly Ancient Greek (pls, mud, earth, clay).

palsf (genitive paldis); third declension

Third declension.

Inherited from a metathesised Vulgar Latin form *padule

From Proto-Italic *pkslos, from Proto-Indo-European *peh-slos, from *peh-. See related terms.

plusm (genitive pli); second declension

Second declension.

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palus – Wiktionary

Planetary science – Wikipedia

Planetary science or, more rarely, planetology, is the scientific study of planets (including Earth), moons, and planetary systems (in particular those of the Solar System) and the processes that form them. It studies objects ranging in size from micrometeoroids to gas giants, aiming to determine their composition, dynamics, formation, interrelations and history. It is a strongly interdisciplinary field, originally growing from astronomy and earth science,[1] but which now incorporates many disciplines, including planetary geology (together with geochemistry and geophysics), cosmochemistry, atmospheric science, oceanography, hydrology, theoretical planetary science, glaciology, and exoplanetology.[1] Allied disciplines include space physics, when concerned with the effects of the Sun on the bodies of the Solar System, and astrobiology.

There are interrelated observational and theoretical branches of planetary science. Observational research can involve a combination of space exploration, predominantly with robotic spacecraft missions using remote sensing, and comparative, experimental work in Earth-based laboratories. The theoretical component involves considerable computer simulation and mathematical modelling.

Planetary scientists are generally located in the astronomy and physics or Earth sciences departments of universities or research centres, though there are several purely planetary science institutes worldwide. There are several major conferences each year, and a wide range of peer-reviewed journals. In the case of some exclusive planetary scientists, many of whom are in relation to the study of dark matter, they will seek a private research centre and often initiate partnership research tasks.

The history of planetary science may be said to have begun with the Ancient Greek philosopher Democritus, who is reported by Hippolytus as saying

The ordered worlds are boundless and differ in size, and that in some there is neither sun nor moon, but that in others, both are greater than with us, and yet with others more in number. And that the intervals between the ordered worlds are unequal, here more and there less, and that some increase, others flourish and others decay, and here they come into being and there they are eclipsed. But that they are destroyed by colliding with one another. And that some ordered worlds are bare of animals and plants and all water.[2]

In more modern times, planetary science began in astronomy, from studies of the unresolved planets. In this sense, the original planetary astronomer would be Galileo, who discovered the four largest moons of Jupiter, the mountains on the Moon, and first observed the rings of Saturn, all objects of intense later study. Galileo’s study of the lunar mountains in 1609 also began the study of extraterrestrial landscapes: his observation “that the Moon certainly does not possess a smooth and polished surface” suggested that it and other worlds might appear “just like the face of the Earth itself”.[3]

Advances in telescope construction and instrumental resolution gradually allowed increased identification of the atmospheric and surface details of the planets. The Moon was initially the most heavily studied, as it always exhibited details on its surface, due to its proximity to the Earth, and the technological improvements gradually produced more detailed lunar geological knowledge. In this scientific process, the main instruments were astronomical optical telescopes (and later radio telescopes) and finally robotic exploratory spacecraft.

The Solar System has now been relatively well-studied, and a good overall understanding of the formation and evolution of this planetary system exists. However, there are large numbers of unsolved questions,[4] and the rate of new discoveries is very high, partly due to the large number of interplanetary spacecraft currently exploring the Solar System.

This is both an observational and a theoretical science. Observational researchers are predominantly concerned with the study of the small bodies of the Solar System: those that are observed by telescopes, both optical and radio, so that characteristics of these bodies such as shape, spin, surface materials and weathering are determined, and the history of their formation and evolution can be understood.

Theoretical planetary astronomy is concerned with dynamics: the application of the principles of celestial mechanics to the Solar System and extrasolar planetary systems.

The best known research topics of planetary geology deal with the planetary bodies in the near vicinity of the Earth: the Moon, and the two neighbouring planets: Venus and Mars. Of these, the Moon was studied first, using methods developed earlier on the Earth.

Geomorphology studies the features on planetary surfaces and reconstructs the history of their formation, inferring the physical processes that acted on the surface. Planetary geomorphology includes the study of several classes of surface features:

The history of a planetary surface can be deciphered by mapping features from top to bottom according to their deposition sequence, as first determined on terrestrial strata by Nicolas Steno. For example, stratigraphic mapping prepared the Apollo astronauts for the field geology they would encounter on their lunar missions. Overlapping sequences were identified on images taken by the Lunar Orbiter program, and these were used to prepare a lunar stratigraphic column and geological map of the Moon.

One of the main problems when generating hypotheses on the formation and evolution of objects in the Solar System is the lack of samples that can be analysed in the laboratory, where a large suite of tools are available and the full body of knowledge derived from terrestrial geology can be brought to bear. Direct samples from the Moon, asteroids and Mars are present on Earth, removed from their parent bodies and delivered as meteorites. Some of these have suffered contamination from the oxidising effect of Earth’s atmosphere and the infiltration of the biosphere, but those meteorites collected in the last few decades from Antarctica are almost entirely pristine.

The different types of meteorites that originate from the asteroid belt cover almost all parts of the structure of differentiated bodies: meteorites even exist that come from the core-mantle boundary (pallasites). The combination of geochemistry and observational astronomy has also made it possible to trace the HED meteorites back to a specific asteroid in the main belt, 4 Vesta.

The comparatively few known Martian meteorites have provided insight into the geochemical composition of the Martian crust, although the unavoidable lack of information about their points of origin on the diverse Martian surface has meant that they do not provide more detailed constraints on theories of the evolution of the Martian lithosphere.[5] As of July 24, 2013 65 samples of Martian meteorites have been discovered on Earth. Many were found in either Antarctica or the Sahara Desert.

During the Apollo era, in the Apollo program, 384 kilograms of lunar samples were collected and transported to the Earth, and 3 Soviet Luna robots also delivered regolith samples from the Moon. These samples provide the most comprehensive record of the composition of any Solar System body beside the Earth. The numbers of lunar meteorites are growing quickly in the last few years [6] as ofApril 2008 there are 54 meteorites that have been officially classified as lunar.Eleven of these are from the US Antarctic meteorite collection, 6 are from the JapaneseAntarctic meteorite collection, and the other 37 are from hot desert localities in Africa,Australia, and the Middle East. The total mass of recognized lunar meteorites is close to50kg.

Space probes made it possible to collect data in not only the visible light region, but in other areas of the electromagnetic spectrum. The planets can be characterized by their force fields: gravity and their magnetic fields, which are studied through geophysics and space physics.

Measuring the changes in acceleration experienced by spacecraft as they orbit has allowed fine details of the gravity fields of the planets to be mapped. For example, in the 1970s, the gravity field disturbances above lunar maria were measured through lunar orbiters, which led to the discovery of concentrations of mass, mascons, beneath the Imbrium, Serenitatis, Crisium, Nectaris and Humorum basins.

If a planet’s magnetic field is sufficiently strong, its interaction with the solar wind forms a magnetosphere around a planet. Early space probes discovered the gross dimensions of the terrestrial magnetic field, which extends about 10 Earth radii towards the Sun. The solar wind, a stream of charged particles, streams out and around the terrestrial magnetic field, and continues behind the magnetic tail, hundreds of Earth radii downstream. Inside the magnetosphere, there are relatively dense regions of solar wind particles, the Van Allen radiation belts.

Geophysics includes seismology and tectonophysics, geophysical fluid dynamics, mineral physics, geodynamics, mathematical geophysics, and geophysical surveying.

Planetary geodesy, (also known as planetary geodetics) deals with the measurement and representation of the planets of the Solar System, their gravitational fields and geodynamic phenomena (polar motion in three-dimensional, time-varying space. The science of geodesy has elements of both astrophysics and planetary sciences. The shape of the Earth is to a large extent the result of its rotation, which causes its equatorial bulge, and the competition of geologic processes such as the collision of plates and of vulcanism, resisted by the Earth’s gravity field. These principles can be applied to the solid surface of Earth (orogeny; Few mountains are higher than 10km (6mi), few deep sea trenches deeper than that because quite simply, a mountain as tall as, for example, 15km (9mi), would develop so much pressure at its base, due to gravity, that the rock there would become plastic, and the mountain would slump back to a height of roughly 10km (6mi) in a geologically insignificant time. Some or all of these geologic principles can be applied to other planets besides Earth. For instance on Mars, whose surface gravity is much less, the largest volcano, Olympus Mons, is 27km (17mi) high at its peak, a height that could not be maintained on Earth. The Earth geoid is essentially the figure of the Earth abstracted from its topographic features. Therefore, the Mars geoid is essentially the figure of Mars abstracted from its topographic features. Surveying and mapping are two important fields of application of geodesy.

The atmosphere is an important transitional zone between the solid planetary surface and the higher rarefied ionizing and radiation belts. Not all planets have atmospheres: their existence depends on the mass of the planet, and the planet’s distance from the Sun too distant and frozen atmospheres occur. Besides the four gas giant planets, almost all of the terrestrial planets (Earth, Venus, and Mars) have significant atmospheres. Two moons have significant atmospheres: Saturn’s moon Titan and Neptune’s moon Triton. A tenuous atmosphere exists around Mercury.

The effects of the rotation rate of a planet about its axis can be seen in atmospheric streams and currents. Seen from space, these features show as bands and eddies in the cloud system, and are particularly visible on Jupiter and Saturn.

Planetary science frequently makes use of the method of comparison to give a greater understanding of the object of study. This can involve comparing the dense atmospheres of Earth and Saturn’s moon Titan, the evolution of outer Solar System objects at different distances from the Sun, or the geomorphology of the surfaces of the terrestrial planets, to give only a few examples.

The main comparison that can be made is to features on the Earth, as it is much more accessible and allows a much greater range of measurements to be made. Earth analogue studies are particularly common in planetary geology, geomorphology, and also in atmospheric science.

Smaller workshops and conferences on particular fields occur worldwide throughout the year.

This non-exhaustive list includes those institutions and universities with major groups of people working in planetary science. Alphabetical order is used.

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Planetary science – Wikipedia

UC San Diego NanoEngineering Department

The NanoEngineering program has received accreditation by the Accreditation Commission of ABET, the global accreditor of college and university programs in applied and natural science, computing, engineering and engineering technology. UC San Diego’s NanoEngineering program is the first of its kind in the nation to receive this accreditation. Our NanoEngineering students can feel confident that their education meets global standards and that they will be prepared to enter the workforce worldwide.

ABET accreditation assures that programs meet standards to produce graduates ready to enter critical technical fields that are leading the way in innovation and emerging technologies, and anticipating the welfare and safety needs of the public. Please visit the ABET website for more information on why accreditation matters.

Congratulations to the NanoEngineering department and students!

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UC San Diego NanoEngineering Department

Nanoengineering – Wikipedia

Nanoengineering is the practice of engineering on the nanoscale. It derives its name from the nanometre, a unit of measurement equalling one billionth of a meter.

Nanoengineering is largely a synonym for nanotechnology, but emphasizes the engineering rather than the pure science aspects of the field.

The first nanoengineering program was started at the University of Toronto within the Engineering Science program as one of the options of study in the final years. In 2003, the Lund Institute of Technology started a program in Nanoengineering. In 2004, the College of Nanoscale Science and Engineering at SUNY Polytechnic Institute was established on the campus of the University at Albany. In 2005, the University of Waterloo established a unique program which offers a full degree in Nanotechnology Engineering. [1] Louisiana Tech University started the first program in the U.S. in 2005. In 2006 the University of Duisburg-Essen started a Bachelor and a Master program NanoEngineering. [2] Unlike early NanoEngineering programs, the first Nanoengineering Department in the world, offering both undergraduate and graduate degrees, was established by the University of California, San Diego in 2007.In 2009, the University of Toronto began offering all Options of study in Engineering Science as degrees, bringing the second nanoengineering degree to Canada. Rice University established in 2016 a Department of Materials Science and NanoEngineering (MSNE).DTU Nanotech – the Department of Micro- and Nanotechnology – is a department at the Technical University of Denmark established in 1990.

In 2013, Wayne State University began offering a Nanoengineering Undergraduate Certificate Program, which is funded by a Nanoengineering Undergraduate Education (NUE) grant from the National Science Foundation. The primary goal is to offer specialized undergraduate training in nanotechnology. Other goals are: 1) to teach emerging technologies at the undergraduate level, 2) to train a new adaptive workforce, and 3) to retrain working engineers and professionals.[3]

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Nanoengineering – Wikipedia

Undergraduate Degree Programs | NanoEngineering

The Department of NanoEngineering offers undergraduate programs leading to theB.S. degreesinNanoengineeringandChemical Engineering. The Chemical Engineering and NanoEngineering undergraduate programs areaccredited by the Engineering Accreditation Commission of ABET. The undergraduate degree programs focus on integrating the various sciences and engineering disciplines necessary for successful careers in the evolving nanotechnology industry.These two degree programshave very different requirements and are described in separate sections.

B.S. NanoEngineering

TheNanoEngineering Undergraduate Program became effective Fall 2010.Thismajor focuses on nanoscale science, engineering, and technology that have the potential to make valuable advances in different areas that include, to name a few, new materials, biology and medicine, energy conversion, sensors, and environmental remediation. The program includes affiliated faculty from the Department of NanoEngineering, Department of Mechanical and Aerospace Engineering, Department of Chemistry and Biochemistry, and the Department of Bioengineering. The NanoEngineering undergraduate program is tailored to provide breadth and flexibility by taking advantage of the strength of basic sciences and other engineering disciplines at UC San Diego. The intention is to graduate nanoengineers who are multidisciplinary and can work in a broad spectrum of industries.

B.S. Chemical Engineering

The Chemical Engineering undergraduate program is housed within the NanoEngineering Department. The program is made up of faculty from the Department of Mechanical and Aerospace Engineering, Department of Chemistry and Biochemistry, the Department of Bioengineering and the Department of NanoEngineering. The curricula at both the undergraduate and graduate levels are designed to support and foster chemical engineering as a profession that interfaces engineering and all aspects of basic sciences (physics, chemistry, and biology). As of Fall 2008, the Department of NanoEngineering has taken over the administration of the B.S. degree in Chemical Engineering.

Academic Advising

Upon admission to the major, students should consult the catalog or NanoEngineering website for their program of study, and their undergraduate/graduate advisor if they have questions. Because some course and/or curricular changes may be made every year, it is imperative that students consult with the departments student affairs advisors on an annual basis.

Students can meet with the academic advisors during walk-in hours, schedule an appointment, or send messages through the Virtual Advising Center (VAC).

Program Alterations/Exceptions to Requirements

Variations from or exceptions to any program or course requirements are possible only if the Undergraduate Affairs Committee approves a petition before the courses in question are taken.

Independent Study

Students may take NANO 199 or CENG 199, Independent Study for Undergraduates, under the guidance of a NANO or CENG faculty member. This course is taken as an elective on a P/NP basis. Under very restrictive conditions, however, it may be used to satisfy upper-division Technical Elective or Nanoengineering Elective course requirements for the major. Students interested in this alternative must have completed at least 90 units and earned a UCSD cumulative GPA of 3.0 or better. Eligible students must identify a faculty member with whom they wish to work and propose a two-quarter research or study topic. Please visit the Student Affairs office for more information.

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Undergraduate Degree Programs | NanoEngineering

NETS – What are Nanoengineering and Nanotechnology?

is one billionth of a meter, or three to five atoms in width. It would take approximately 40,000 nanometers lined up in a row to equal the width of a human hair. NanoEngineering concerns itself with manipulating processes that occur on the scale of 1-100 nanometers.

The general term, nanotechnology, is sometimes used to refer to common products that have improved properties due to being fortified with nanoscale materials. One example is nano-improved tooth-colored enamel, as used by dentists for fillings. The general use of the term nanotechnology then differs from the more specific sciences that fall under its heading.

NanoEngineering is an interdisciplinary science that builds biochemical structures smaller than bacterium, which function like microscopic factories. This is possible by utilizing basic biochemical processes at the atomic or molecular level. In simple terms, molecules interact through natural processes, and NanoEngineering takes advantage of those processes by direct manipulation.

SOURCE:http://www.wisegeek.com/what-is-nanoengineering.htm

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NETS – What are Nanoengineering and Nanotechnology?

About the NANO-ENGINEERING FLAGSHIP

Turning the NaI concept into reality necessitates an extraordinary and long-term effort. This requires the integration of nanoelectronics, nanophotonics, nanophononics, nanospintronics, topological effects, as well as the physics and chemistry of materials. This also requires operations in an extremely broad range of science and technology, including Microwaves, Millimeter waves, TeraHertz, Infrared and Optics, and will exploit various excitations, such as surface waves, spin waves, phonons, electrons, photons, plasmons, and their hybrids, for sensing, information processing and storage. Integrating

This high level of integration, which goes beyond individual functionalities, components and devices and requires cooperation across a range of disciplines, makes the Nano Engineering Flagship unique in its approach. It will be crucial in tackling the 6 strategic challenges identified as:

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About the NANO-ENGINEERING FLAGSHIP

The NANO-ENGINEERING FLAGSHIP initiative

Nano-Engineering introduces a novel key-enabling non-invasive broadband technology, the Nano-engineered Interface (NaI), realising omni -connectivity and putting humans and their interactions at the center of the future digital society.Omni-connectivity encompasses real-time communication, sensing, monitoring, and data processing among humans, objects, and their environment. The vision of Omni-connectivity englobes people in a new sphere of extremely simplified, intuitive and natural communication.The Nano-engineered Interface (NaI) a non-invasive wireless ultraflat functional system will make this possible. NaI will be applicable to any surface on any physical item and thereby exponentially diversify and increase connections among humans, wearables, vehicles, and everyday objects. NaI will communicate with other NaI-networks from local up to satellites by using the whole frequency spectrum from microwave frequency to optics

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The NANO-ENGINEERING FLAGSHIP initiative

Planetary science – Wikipedia

Planetary science or, more rarely, planetology, is the scientific study of planets (including Earth), moons, and planetary systems (in particular those of the Solar System) and the processes that form them. It studies objects ranging in size from micrometeoroids to gas giants, aiming to determine their composition, dynamics, formation, interrelations and history. It is a strongly interdisciplinary field, originally growing from astronomy and earth science,[1] but which now incorporates many disciplines, including planetary geology (together with geochemistry and geophysics), cosmochemistry, atmospheric science, oceanography, hydrology, theoretical planetary science, glaciology, and exoplanetology.[1] Allied disciplines include space physics, when concerned with the effects of the Sun on the bodies of the Solar System, and astrobiology.

There are interrelated observational and theoretical branches of planetary science. Observational research can involve a combination of space exploration, predominantly with robotic spacecraft missions using remote sensing, and comparative, experimental work in Earth-based laboratories. The theoretical component involves considerable computer simulation and mathematical modelling.

Planetary scientists are generally located in the astronomy and physics or Earth sciences departments of universities or research centres, though there are several purely planetary science institutes worldwide. There are several major conferences each year, and a wide range of peer-reviewed journals. In the case of some exclusive planetary scientists, many of whom are in relation to the study of dark matter, they will seek a private research centre and often initiate partnership research tasks.

The history of planetary science may be said to have begun with the Ancient Greek philosopher Democritus, who is reported by Hippolytus as saying

The ordered worlds are boundless and differ in size, and that in some there is neither sun nor moon, but that in others, both are greater than with us, and yet with others more in number. And that the intervals between the ordered worlds are unequal, here more and there less, and that some increase, others flourish and others decay, and here they come into being and there they are eclipsed. But that they are destroyed by colliding with one another. And that some ordered worlds are bare of animals and plants and all water.[2]

In more modern times, planetary science began in astronomy, from studies of the unresolved planets. In this sense, the original planetary astronomer would be Galileo, who discovered the four largest moons of Jupiter, the mountains on the Moon, and first observed the rings of Saturn, all objects of intense later study. Galileo’s study of the lunar mountains in 1609 also began the study of extraterrestrial landscapes: his observation “that the Moon certainly does not possess a smooth and polished surface” suggested that it and other worlds might appear “just like the face of the Earth itself”.[3]

Advances in telescope construction and instrumental resolution gradually allowed increased identification of the atmospheric and surface details of the planets. The Moon was initially the most heavily studied, as it always exhibited details on its surface, due to its proximity to the Earth, and the technological improvements gradually produced more detailed lunar geological knowledge. In this scientific process, the main instruments were astronomical optical telescopes (and later radio telescopes) and finally robotic exploratory spacecraft.

The Solar System has now been relatively well-studied, and a good overall understanding of the formation and evolution of this planetary system exists. However, there are large numbers of unsolved questions,[4] and the rate of new discoveries is very high, partly due to the large number of interplanetary spacecraft currently exploring the Solar System.

This is both an observational and a theoretical science. Observational researchers are predominantly concerned with the study of the small bodies of the Solar System: those that are observed by telescopes, both optical and radio, so that characteristics of these bodies such as shape, spin, surface materials and weathering are determined, and the history of their formation and evolution can be understood.

Theoretical planetary astronomy is concerned with dynamics: the application of the principles of celestial mechanics to the Solar System and extrasolar planetary systems.

The best known research topics of planetary geology deal with the planetary bodies in the near vicinity of the Earth: the Moon, and the two neighbouring planets: Venus and Mars. Of these, the Moon was studied first, using methods developed earlier on the Earth.

Geomorphology studies the features on planetary surfaces and reconstructs the history of their formation, inferring the physical processes that acted on the surface. Planetary geomorphology includes the study of several classes of surface features:

The history of a planetary surface can be deciphered by mapping features from top to bottom according to their deposition sequence, as first determined on terrestrial strata by Nicolas Steno. For example, stratigraphic mapping prepared the Apollo astronauts for the field geology they would encounter on their lunar missions. Overlapping sequences were identified on images taken by the Lunar Orbiter program, and these were used to prepare a lunar stratigraphic column and geological map of the Moon.

One of the main problems when generating hypotheses on the formation and evolution of objects in the Solar System is the lack of samples that can be analysed in the laboratory, where a large suite of tools are available and the full body of knowledge derived from terrestrial geology can be brought to bear. Direct samples from the Moon, asteroids and Mars are present on Earth, removed from their parent bodies and delivered as meteorites. Some of these have suffered contamination from the oxidising effect of Earth’s atmosphere and the infiltration of the biosphere, but those meteorites collected in the last few decades from Antarctica are almost entirely pristine.

The different types of meteorites that originate from the asteroid belt cover almost all parts of the structure of differentiated bodies: meteorites even exist that come from the core-mantle boundary (pallasites). The combination of geochemistry and observational astronomy has also made it possible to trace the HED meteorites back to a specific asteroid in the main belt, 4 Vesta.

The comparatively few known Martian meteorites have provided insight into the geochemical composition of the Martian crust, although the unavoidable lack of information about their points of origin on the diverse Martian surface has meant that they do not provide more detailed constraints on theories of the evolution of the Martian lithosphere.[5] As of July 24, 2013 65 samples of Martian meteorites have been discovered on Earth. Many were found in either Antarctica or the Sahara Desert.

During the Apollo era, in the Apollo program, 384 kilograms of lunar samples were collected and transported to the Earth, and 3 Soviet Luna robots also delivered regolith samples from the Moon. These samples provide the most comprehensive record of the composition of any Solar System body beside the Earth. The numbers of lunar meteorites are growing quickly in the last few years [6] as ofApril 2008 there are 54 meteorites that have been officially classified as lunar.Eleven of these are from the US Antarctic meteorite collection, 6 are from the JapaneseAntarctic meteorite collection, and the other 37 are from hot desert localities in Africa,Australia, and the Middle East. The total mass of recognized lunar meteorites is close to50kg.

Space probes made it possible to collect data in not only the visible light region, but in other areas of the electromagnetic spectrum. The planets can be characterized by their force fields: gravity and their magnetic fields, which are studied through geophysics and space physics.

Measuring the changes in acceleration experienced by spacecraft as they orbit has allowed fine details of the gravity fields of the planets to be mapped. For example, in the 1970s, the gravity field disturbances above lunar maria were measured through lunar orbiters, which led to the discovery of concentrations of mass, mascons, beneath the Imbrium, Serenitatis, Crisium, Nectaris and Humorum basins.

If a planet’s magnetic field is sufficiently strong, its interaction with the solar wind forms a magnetosphere around a planet. Early space probes discovered the gross dimensions of the terrestrial magnetic field, which extends about 10 Earth radii towards the Sun. The solar wind, a stream of charged particles, streams out and around the terrestrial magnetic field, and continues behind the magnetic tail, hundreds of Earth radii downstream. Inside the magnetosphere, there are relatively dense regions of solar wind particles, the Van Allen radiation belts.

Geophysics includes seismology and tectonophysics, geophysical fluid dynamics, mineral physics, geodynamics, mathematical geophysics, and geophysical surveying.

Planetary geodesy, (also known as planetary geodetics) deals with the measurement and representation of the planets of the Solar System, their gravitational fields and geodynamic phenomena (polar motion in three-dimensional, time-varying space. The science of geodesy has elements of both astrophysics and planetary sciences. The shape of the Earth is to a large extent the result of its rotation, which causes its equatorial bulge, and the competition of geologic processes such as the collision of plates and of vulcanism, resisted by the Earth’s gravity field. These principles can be applied to the solid surface of Earth (orogeny; Few mountains are higher than 10km (6mi), few deep sea trenches deeper than that because quite simply, a mountain as tall as, for example, 15km (9mi), would develop so much pressure at its base, due to gravity, that the rock there would become plastic, and the mountain would slump back to a height of roughly 10km (6mi) in a geologically insignificant time. Some or all of these geologic principles can be applied to other planets besides Earth. For instance on Mars, whose surface gravity is much less, the largest volcano, Olympus Mons, is 27km (17mi) high at its peak, a height that could not be maintained on Earth. The Earth geoid is essentially the figure of the Earth abstracted from its topographic features. Therefore, the Mars geoid is essentially the figure of Mars abstracted from its topographic features. Surveying and mapping are two important fields of application of geodesy.

The atmosphere is an important transitional zone between the solid planetary surface and the higher rarefied ionizing and radiation belts. Not all planets have atmospheres: their existence depends on the mass of the planet, and the planet’s distance from the Sun too distant and frozen atmospheres occur. Besides the four gas giant planets, almost all of the terrestrial planets (Earth, Venus, and Mars) have significant atmospheres. Two moons have significant atmospheres: Saturn’s moon Titan and Neptune’s moon Triton. A tenuous atmosphere exists around Mercury.

The effects of the rotation rate of a planet about its axis can be seen in atmospheric streams and currents. Seen from space, these features show as bands and eddies in the cloud system, and are particularly visible on Jupiter and Saturn.

Planetary science frequently makes use of the method of comparison to give a greater understanding of the object of study. This can involve comparing the dense atmospheres of Earth and Saturn’s moon Titan, the evolution of outer Solar System objects at different distances from the Sun, or the geomorphology of the surfaces of the terrestrial planets, to give only a few examples.

The main comparison that can be made is to features on the Earth, as it is much more accessible and allows a much greater range of measurements to be made. Earth analogue studies are particularly common in planetary geology, geomorphology, and also in atmospheric science.

Smaller workshops and conferences on particular fields occur worldwide throughout the year.

This non-exhaustive list includes those institutions and universities with major groups of people working in planetary science. Alphabetical order is used.

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Planetary science – Wikipedia

Eve online planetary interaction

Materials

EVE Online and the EVE logo are the registered trademarks of CCP hf. All rights are reserved worldwide. All other trademarks are the property of their respective owners. EVE Online, the EVE logo, EVE and all associated logos and designs are the intellectual property of CCP hf. All artwork, screenshots, characters, vehicles, storylines, world facts or other recognizable features of the intellectual property relating to these trademarks are likewise the intellectual property of CCP hf. CCP hf. has granted permission to [insert your name or site name] to use EVE Online and all associated logos and designs for promotional and information purposes on its website but does not endorse, and is not in any way affiliated with, [insert name or site name]. CCP is in no way responsible for the content on or functioning of this website, nor can it be liable for any damage arising from the use of this website.

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Eve online planetary interaction

palus – Wiktionary

English[edit]Etymology 1[edit]

From Latin plus (stake, post). Doublet of pole.

palus (plural pali)

From Latin pals (marsh, swamp).

palus (plural paludes)

palus?

From Proto-Italic *palts, *pald-, from Proto-Indo-European *pelHk-iH-h, related to Latvian pelce (puddle), Lithuanian pelk (marsh), Sanskrit (palvala, pool, pond), and possibly Ancient Greek (pls, mud, earth, clay).

palsf (genitive paldis); third declension

Third declension.

Inherited from a metathesised Vulgar Latin form *padule

From Proto-Italic *pkslos, from Proto-Indo-European *peh-slos, from *peh-. See related terms.

plusm (genitive pli); second declension

Second declension.

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palus – Wiktionary

Homepage INAF English

On October 14th 2015, the Italian Ministry of Education, University and Research (MIUR) appointed Professor Nicol D’Amico as President of the Italian National Institute for Astrophysics (INAF). Full professor in Astrophysics at University of Cagliari, D’Amico has been previously director of the INAF Astronomical Observatory in Cagliari and the director of the Sardinia Radio Telescope (SRT) Project.

Below, the latest news on the president:

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Homepage INAF English

Eve online planetary interaction

Materials

EVE Online and the EVE logo are the registered trademarks of CCP hf. All rights are reserved worldwide. All other trademarks are the property of their respective owners. EVE Online, the EVE logo, EVE and all associated logos and designs are the intellectual property of CCP hf. All artwork, screenshots, characters, vehicles, storylines, world facts or other recognizable features of the intellectual property relating to these trademarks are likewise the intellectual property of CCP hf. CCP hf. has granted permission to [insert your name or site name] to use EVE Online and all associated logos and designs for promotional and information purposes on its website but does not endorse, and is not in any way affiliated with, [insert name or site name]. CCP is in no way responsible for the content on or functioning of this website, nor can it be liable for any damage arising from the use of this website.

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Eve online planetary interaction

Planetary science – Wikipedia

Planetary science or, more rarely, planetology, is the scientific study of planets (including Earth), moons, and planetary systems (in particular those of the Solar System) and the processes that form them. It studies objects ranging in size from micrometeoroids to gas giants, aiming to determine their composition, dynamics, formation, interrelations and history. It is a strongly interdisciplinary field, originally growing from astronomy and earth science,[1] but which now incorporates many disciplines, including planetary geology (together with geochemistry and geophysics), cosmochemistry, atmospheric science, oceanography, hydrology, theoretical planetary science, glaciology, and exoplanetology.[1] Allied disciplines include space physics, when concerned with the effects of the Sun on the bodies of the Solar System, and astrobiology.

There are interrelated observational and theoretical branches of planetary science. Observational research can involve a combination of space exploration, predominantly with robotic spacecraft missions using remote sensing, and comparative, experimental work in Earth-based laboratories. The theoretical component involves considerable computer simulation and mathematical modelling.

Planetary scientists are generally located in the astronomy and physics or Earth sciences departments of universities or research centres, though there are several purely planetary science institutes worldwide. There are several major conferences each year, and a wide range of peer-reviewed journals. In the case of some exclusive planetary scientists, many of whom are in relation to the study of dark matter, they will seek a private research centre and often initiate partnership research tasks.

The history of planetary science may be said to have begun with the Ancient Greek philosopher Democritus, who is reported by Hippolytus as saying

The ordered worlds are boundless and differ in size, and that in some there is neither sun nor moon, but that in others, both are greater than with us, and yet with others more in number. And that the intervals between the ordered worlds are unequal, here more and there less, and that some increase, others flourish and others decay, and here they come into being and there they are eclipsed. But that they are destroyed by colliding with one another. And that some ordered worlds are bare of animals and plants and all water.[2]

In more modern times, planetary science began in astronomy, from studies of the unresolved planets. In this sense, the original planetary astronomer would be Galileo, who discovered the four largest moons of Jupiter, the mountains on the Moon, and first observed the rings of Saturn, all objects of intense later study. Galileo’s study of the lunar mountains in 1609 also began the study of extraterrestrial landscapes: his observation “that the Moon certainly does not possess a smooth and polished surface” suggested that it and other worlds might appear “just like the face of the Earth itself”.[3]

Advances in telescope construction and instrumental resolution gradually allowed increased identification of the atmospheric and surface details of the planets. The Moon was initially the most heavily studied, as it always exhibited details on its surface, due to its proximity to the Earth, and the technological improvements gradually produced more detailed lunar geological knowledge. In this scientific process, the main instruments were astronomical optical telescopes (and later radio telescopes) and finally robotic exploratory spacecraft.

The Solar System has now been relatively well-studied, and a good overall understanding of the formation and evolution of this planetary system exists. However, there are large numbers of unsolved questions,[4] and the rate of new discoveries is very high, partly due to the large number of interplanetary spacecraft currently exploring the Solar System.

This is both an observational and a theoretical science. Observational researchers are predominantly concerned with the study of the small bodies of the Solar System: those that are observed by telescopes, both optical and radio, so that characteristics of these bodies such as shape, spin, surface materials and weathering are determined, and the history of their formation and evolution can be understood.

Theoretical planetary astronomy is concerned with dynamics: the application of the principles of celestial mechanics to the Solar System and extrasolar planetary systems.

The best known research topics of planetary geology deal with the planetary bodies in the near vicinity of the Earth: the Moon, and the two neighbouring planets: Venus and Mars. Of these, the Moon was studied first, using methods developed earlier on the Earth.

Geomorphology studies the features on planetary surfaces and reconstructs the history of their formation, inferring the physical processes that acted on the surface. Planetary geomorphology includes the study of several classes of surface features:

The history of a planetary surface can be deciphered by mapping features from top to bottom according to their deposition sequence, as first determined on terrestrial strata by Nicolas Steno. For example, stratigraphic mapping prepared the Apollo astronauts for the field geology they would encounter on their lunar missions. Overlapping sequences were identified on images taken by the Lunar Orbiter program, and these were used to prepare a lunar stratigraphic column and geological map of the Moon.

One of the main problems when generating hypotheses on the formation and evolution of objects in the Solar System is the lack of samples that can be analysed in the laboratory, where a large suite of tools are available and the full body of knowledge derived from terrestrial geology can be brought to bear. Direct samples from the Moon, asteroids and Mars are present on Earth, removed from their parent bodies and delivered as meteorites. Some of these have suffered contamination from the oxidising effect of Earth’s atmosphere and the infiltration of the biosphere, but those meteorites collected in the last few decades from Antarctica are almost entirely pristine.

The different types of meteorites that originate from the asteroid belt cover almost all parts of the structure of differentiated bodies: meteorites even exist that come from the core-mantle boundary (pallasites). The combination of geochemistry and observational astronomy has also made it possible to trace the HED meteorites back to a specific asteroid in the main belt, 4 Vesta.

The comparatively few known Martian meteorites have provided insight into the geochemical composition of the Martian crust, although the unavoidable lack of information about their points of origin on the diverse Martian surface has meant that they do not provide more detailed constraints on theories of the evolution of the Martian lithosphere.[5] As of July 24, 2013 65 samples of Martian meteorites have been discovered on Earth. Many were found in either Antarctica or the Sahara Desert.

During the Apollo era, in the Apollo program, 384 kilograms of lunar samples were collected and transported to the Earth, and 3 Soviet Luna robots also delivered regolith samples from the Moon. These samples provide the most comprehensive record of the composition of any Solar System body beside the Earth. The numbers of lunar meteorites are growing quickly in the last few years [6] as ofApril 2008 there are 54 meteorites that have been officially classified as lunar.Eleven of these are from the US Antarctic meteorite collection, 6 are from the JapaneseAntarctic meteorite collection, and the other 37 are from hot desert localities in Africa,Australia, and the Middle East. The total mass of recognized lunar meteorites is close to50kg.

Space probes made it possible to collect data in not only the visible light region, but in other areas of the electromagnetic spectrum. The planets can be characterized by their force fields: gravity and their magnetic fields, which are studied through geophysics and space physics.

Measuring the changes in acceleration experienced by spacecraft as they orbit has allowed fine details of the gravity fields of the planets to be mapped. For example, in the 1970s, the gravity field disturbances above lunar maria were measured through lunar orbiters, which led to the discovery of concentrations of mass, mascons, beneath the Imbrium, Serenitatis, Crisium, Nectaris and Humorum basins.

If a planet’s magnetic field is sufficiently strong, its interaction with the solar wind forms a magnetosphere around a planet. Early space probes discovered the gross dimensions of the terrestrial magnetic field, which extends about 10 Earth radii towards the Sun. The solar wind, a stream of charged particles, streams out and around the terrestrial magnetic field, and continues behind the magnetic tail, hundreds of Earth radii downstream. Inside the magnetosphere, there are relatively dense regions of solar wind particles, the Van Allen radiation belts.

Geophysics includes seismology and tectonophysics, geophysical fluid dynamics, mineral physics, geodynamics, mathematical geophysics, and geophysical surveying.

Planetary geodesy, (also known as planetary geodetics) deals with the measurement and representation of the planets of the Solar System, their gravitational fields and geodynamic phenomena (polar motion in three-dimensional, time-varying space. The science of geodesy has elements of both astrophysics and planetary sciences. The shape of the Earth is to a large extent the result of its rotation, which causes its equatorial bulge, and the competition of geologic processes such as the collision of plates and of vulcanism, resisted by the Earth’s gravity field. These principles can be applied to the solid surface of Earth (orogeny; Few mountains are higher than 10km (6mi), few deep sea trenches deeper than that because quite simply, a mountain as tall as, for example, 15km (9mi), would develop so much pressure at its base, due to gravity, that the rock there would become plastic, and the mountain would slump back to a height of roughly 10km (6mi) in a geologically insignificant time. Some or all of these geologic principles can be applied to other planets besides Earth. For instance on Mars, whose surface gravity is much less, the largest volcano, Olympus Mons, is 27km (17mi) high at its peak, a height that could not be maintained on Earth. The Earth geoid is essentially the figure of the Earth abstracted from its topographic features. Therefore, the Mars geoid is essentially the figure of Mars abstracted from its topographic features. Surveying and mapping are two important fields of application of geodesy.

The atmosphere is an important transitional zone between the solid planetary surface and the higher rarefied ionizing and radiation belts. Not all planets have atmospheres: their existence depends on the mass of the planet, and the planet’s distance from the Sun too distant and frozen atmospheres occur. Besides the four gas giant planets, almost all of the terrestrial planets (Earth, Venus, and Mars) have significant atmospheres. Two moons have significant atmospheres: Saturn’s moon Titan and Neptune’s moon Triton. A tenuous atmosphere exists around Mercury.

The effects of the rotation rate of a planet about its axis can be seen in atmospheric streams and currents. Seen from space, these features show as bands and eddies in the cloud system, and are particularly visible on Jupiter and Saturn.

Planetary science frequently makes use of the method of comparison to give a greater understanding of the object of study. This can involve comparing the dense atmospheres of Earth and Saturn’s moon Titan, the evolution of outer Solar System objects at different distances from the Sun, or the geomorphology of the surfaces of the terrestrial planets, to give only a few examples.

The main comparison that can be made is to features on the Earth, as it is much more accessible and allows a much greater range of measurements to be made. Earth analogue studies are particularly common in planetary geology, geomorphology, and also in atmospheric science.

Smaller workshops and conferences on particular fields occur worldwide throughout the year.

This non-exhaustive list includes those institutions and universities with major groups of people working in planetary science. Alphabetical order is used.

See more here:

Planetary science – Wikipedia

Homepage INAF English

On October 14th 2015, the Italian Ministry of Education, University and Research (MIUR) appointed Professor Nicol D’Amico as President of the Italian National Institute for Astrophysics (INAF). Full professor in Astrophysics at University of Cagliari, D’Amico has been previously director of the INAF Astronomical Observatory in Cagliari and the director of the Sardinia Radio Telescope (SRT) Project.

Below, the latest news on the president:

Read the original post:

Homepage INAF English

palus – Wiktionary

English[edit]Etymology 1[edit]

From Latin plus (stake, post). Doublet of pole.

palus (plural pali)

From Latin pals (marsh, swamp).

palus (plural paludes)

palus?

From Proto-Italic *palts, *pald-, from Proto-Indo-European *pelHk-iH-h, related to Latvian pelce (puddle), Lithuanian pelk (marsh), Sanskrit (palvala, pool, pond), and possibly Ancient Greek (pls, mud, earth, clay).

palsf (genitive paldis); third declension

Third declension.

Inherited from a metathesised Vulgar Latin form *padule

From Proto-Italic *pkslos, from Proto-Indo-European *peh-slos, from *peh-. See related terms.

plusm (genitive pli); second declension

Second declension.

View post:

palus – Wiktionary

AI Dreamed Up These Nightmare Fuel Halloween Masks

Nightmare Fuel

Someone programmed an AI to dream up Halloween masks, and the results are absolute nightmare fuel. Seriously, just look at some of these things.

“What’s so scary or unsettling about it is that it’s not so detailed that it shows you everything,” said Matt Reed, the creator of the masks, in an interview with New Scientist. “It leaves just enough open for your imagination to connect the dots.”

A selection of masks featured on Reed’s twitter. Credit: Matt Reed/Twitter

Creative Horror

To create the masks, Reed — whose day job is as a technologist at a creative agency called redpepper — fed an open source AI tool 5,000 pictures of Halloween masks he sourced from Google Images. He then instructed the tool to generate its own masks.

The fun and spooky project is yet another sign that AI is coming into its own as a creative tool. Just yesterday, a portrait generated by a similar system fetched more than $400,000 at a prominent British auction house.

And Reed’s masks are evocative. Here at the Byte, if we looked through the peephole and saw one of these on a trick or treater, we might not open our door.

READ MORE: AI Designed These Halloween Masks and They Are Absolutely Terrifying [New Scientist]

More on AI-generated art: Generated Art Will Go on Sale Alongside Human-Made Works This Fall

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AI Dreamed Up These Nightmare Fuel Halloween Masks

Robot Security Guards Will Constantly Nag Spectators at the Tokyo Olympics

Over and Over

“The security robot is patrolling. Ding-ding. Ding-ding. The security robot is patrolling. Ding-ding. Ding-ding.”

That’s what Olympic attendees will hear ad nauseam when they step onto the platforms of Tokyo’s train stations in 2020. The source: Perseusbot, a robot security guard Japanese developers unveiled to the press on Thursday.

Observe and Report

According to reporting by Kyodo News, the purpose of the AI-powered Perseusbot is to lower the burden on the stations’ staff when visitors flood Tokyo during the 2020 Olympics.

The robot is roughly 5.5 feet tall and equipped with security cameras that allow it to note suspicious behaviors, such as signs of violence breaking out or unattended packages, as it autonomous patrols the area. It can then alert security staff to the issues by sending notifications directly to their smart phones.

Prior Prepration

Just like the athletes who will head to Tokyo in 2020, Perseusbot already has a training program in the works — it’ll patrol Tokyo’s Seibu Shinjuku Station from November 26 to 30. This dry run should give the bot’s developers a chance to work out any kinks before 2020.

If all goes as hoped, the bot will be ready to annoy attendees with its incessant chant before the Olympic torch is lit. And, you know, keep everyone safe, too.

READ MORE: Robot Station Security Guard Unveiled Ahead of 2020 Tokyo Olympics [Kyodo News]

More robot security guards: Robot Security Guards Are Just the Beginning

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Robot Security Guards Will Constantly Nag Spectators at the Tokyo Olympics


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