2011-2 Sidereal-Times
Total Page:16
File Type:pdf, Size:1020Kb
Load more
Recommended publications
-
Curiosity's Candidate Field Site in Gale Crater, Mars
Curiosity’s Candidate Field Site in Gale Crater, Mars K. S. Edgett – 27 September 2010 Simulated view from Curiosity rover in landing ellipse looking toward the field area in Gale; made using MRO CTX stereopair images; no vertical exaggeration. The mound is ~15 km away 4th MSL Landing Site Workshop, 27–29 September 2010 in this view. Note that one would see Gale’s SW wall in the distant background if this were Edgett, 1 actually taken by the Mastcams on Mars. Gale Presents Perhaps the Thickest and Most Diverse Exposed Stratigraphic Section on Mars • Gale’s Mound appears to present the thickest and most diverse exposed stratigraphic section on Mars that we can hope access in this decade. • Mound has ~5 km of stratified rock. (That’s 3 miles!) • There is no evidence that volcanism ever occurred in Gale. • Mound materials were deposited as sediment. • Diverse materials are present. • Diverse events are recorded. – Episodes of sedimentation and lithification and diagenesis. – Episodes of erosion, transport, and re-deposition of mound materials. 4th MSL Landing Site Workshop, 27–29 September 2010 Edgett, 2 Gale is at ~5°S on the “north-south dichotomy boundary” in the Aeolis and Nepenthes Mensae Region base map made by MSSS for National Geographic (February 2001); from MOC wide angle images and MOLA topography 4th MSL Landing Site Workshop, 27–29 September 2010 Edgett, 3 Proposed MSL Field Site In Gale Crater Landing ellipse - very low elevation (–4.5 km) - shown here as 25 x 20 km - alluvium from crater walls - drive to mound Anderson & Bell -
Phobos, Deimos: Formation and Evolution Alex Soumbatov-Gur
Phobos, Deimos: Formation and Evolution Alex Soumbatov-Gur To cite this version: Alex Soumbatov-Gur. Phobos, Deimos: Formation and Evolution. [Research Report] Karpov institute of physical chemistry. 2019. hal-02147461 HAL Id: hal-02147461 https://hal.archives-ouvertes.fr/hal-02147461 Submitted on 4 Jun 2019 HAL is a multi-disciplinary open access L’archive ouverte pluridisciplinaire HAL, est archive for the deposit and dissemination of sci- destinée au dépôt et à la diffusion de documents entific research documents, whether they are pub- scientifiques de niveau recherche, publiés ou non, lished or not. The documents may come from émanant des établissements d’enseignement et de teaching and research institutions in France or recherche français ou étrangers, des laboratoires abroad, or from public or private research centers. publics ou privés. Phobos, Deimos: Formation and Evolution Alex Soumbatov-Gur The moons are confirmed to be ejected parts of Mars’ crust. After explosive throwing out as cone-like rocks they plastically evolved with density decays and materials transformations. Their expansion evolutions were accompanied by global ruptures and small scale rock ejections with concurrent crater formations. The scenario reconciles orbital and physical parameters of the moons. It coherently explains dozens of their properties including spectra, appearances, size differences, crater locations, fracture symmetries, orbits, evolution trends, geologic activity, Phobos’ grooves, mechanism of their origin, etc. The ejective approach is also discussed in the context of observational data on near-Earth asteroids, main belt asteroids Steins, Vesta, and Mars. The approach incorporates known fission mechanism of formation of miniature asteroids, logically accounts for its outliers, and naturally explains formations of small celestial bodies of various sizes. -
Turbulence and Aeolian Morphodynamics in Craters on Mars: Application to Gale Crater, Landing Site of the Curiosity Rover
16TH EUROPEAN TURBULENCE CONFERENCE, 21-24 AUGUST, 2017, STOCKHOLM,SWEDEN TURBULENCE AND AEOLIAN MORPHODYNAMICS IN CRATERS ON MARS: APPLICATION TO GALE CRATER, LANDING SITE OF THE CURIOSITY ROVER William Anderson1, Gary Kocurek2 & Kenzie Day2 1Mechanical Engineering Dept., Univ. Texas at Dallas, Richardson, Texas, USA 2Dept. Geological Sciences, Jackson School of Geosciences, Univ. Texas at Austin, Austin, Texas, USA Mars is a dry planet with a thin atmosphere. Aeolian processes – wind-driven mobilization of sediment and dust – are the dominant mode of landscape variability on the dessicated landscapes of Mars. Craters are common topographic features on the surface of Mars, and many craters on Mars contain a prominent central mound (NASA’s Curiosity rover was landed in Gale crater, shown in Figure 1a [1], while Figures 1b and 1c show Henry and Korolev crater, respectively). These mounds are composed of sedimentary fill and, therefore, they contain rich information on the evolution of climatic conditions on Mars embodied in the stratigraphic “layering” of sediments. Many other craters no longer house a mound, but contain sediment and dust from which dune fields and other features form (see, for example, Victoria Crater, Figure 1d). Using density-normalized large-eddy simulations, we have modeled turbulent flows over crater-like topographies that feature a central mound. Resultant datasets suggest a deflationary mechanism wherein vortices shed from the upwind crater rim are realigned to conform to the crater profile via stretching and tilting. This was accomplished using three- dimensional datasets (momentum and vorticity) retrieved from LES. As a result, helical vortices occupy the inner region of the crater and, therefore, are primarily responsible for aeolian morphodynamics in the crater (radial katabatic flows are also important to aeolian processes within the crater [2]). -
Exploration of Victoria Crater by the Mars Rover Opportunity
Exploration of Victoria Crater by the Mars Rover Opportunity The Harvard community has made this article openly available. Please share how this access benefits you. Your story matters Citation Squyres, Steven W., Andrew H. Knoll, Raymond E. Arvidson, James W. Ashley, James F. III Bell, Wendy M. Calvin, Philip R. Christensen, et al. 2009. Exploration of Victoria Crater by the Mars rover Opportunity. Science 324(5930): 1058-1061. Published Version doi:10.1126/science.1170355 Citable link http://nrs.harvard.edu/urn-3:HUL.InstRepos:3934552 Terms of Use This article was downloaded from Harvard University’s DASH repository, and is made available under the terms and conditions applicable to Open Access Policy Articles, as set forth at http:// nrs.harvard.edu/urn-3:HUL.InstRepos:dash.current.terms-of- use#OAP Exploration of Victoria Crater by the Rover Opportunity S.W. Squyres1, A.H. Knoll2, R.E. Arvidson3, J.W. Ashley4, J.F. Bell III1, W.M. Calvin5, P.R. Christensen4, B.C. Clark6, B.A. Cohen7, P.A. de Souza Jr.8, L. Edgar9, W.H. Farrand10, I. Fleischer11, R. Gellert12, M.P. Golombek13, J. Grant14, J. Grotzinger9, A. Hayes9, K.E. Herkenhoff15, J.R. Johnson15, B. Jolliff3, G. Klingelhöfer11, A. Knudson4, R. Li16, T.J. McCoy17, S.M. McLennan18, D.W. Ming19, D.W. Mittlefehldt19, R.V. Morris19, J.W. Rice Jr.4, C. Schröder11, R.J. Sullivan1, A. Yen13, R.A. Yingst20 1 Dept. of Astronomy, Space Sciences Bldg., Cornell University, Ithaca, NY 14853, USA 2 Botanical Museum, Harvard University, Cambridge MA 02138, USA 3 Dept. -
Mars Reconnaissance Orbiter and Opportunity Observations Of
PUBLICATIONS Journal of Geophysical Research: Planets RESEARCH ARTICLE Mars Reconnaissance Orbiter and Opportunity 10.1002/2014JE004686 observations of the Burns formation: Crater Key Point: hopping at Meridiani Planum • Hydrated Mg and Ca sulfate Burns formation minerals mapped with MRO R. E. Arvidson1, J. F. Bell III2, J. G. Catalano1, B. C. Clark3, V. K. Fox1, R. Gellert4, J. P. Grotzinger5, and MER data E. A. Guinness1, K. E. Herkenhoff6, A. H. Knoll7, M. G. A. Lapotre5, S. M. McLennan8, D. W. Ming9, R. V. Morris9, S. L. Murchie10, K. E. Powell1, M. D. Smith11, S. W. Squyres12, M. J. Wolff3, and J. J. Wray13 1 2 Correspondence to: Department of Earth and Planetary Sciences, Washington University in Saint Louis, Missouri, USA, School of Earth and Space R. E. Arvidson, Exploration, Arizona State University, Tempe, Arizona, USA, 3Space Science Institute, Boulder, Colorado, USA, 4Department of [email protected] Physics, University of Guelph, Guelph, Ontario, Canada, 5Division of Geological and Planetary Sciences, California Institute of Technology, Pasadena, California, USA, 6U.S. Geological Survey, Astrogeology Science Center, Flagstaff, Arizona, USA, 7 8 Citation: Department of Organismic and Evolutionary Biology, Harvard University, Cambridge, Massachusetts, USA, Department Arvidson, R. E., et al. (2015), Mars of Geosciences, Stony Brook University, Stony Brook, New York, USA, 9NASA Johnson Space Center, Houston, Texas, USA, Reconnaissance Orbiter and Opportunity 10Applied Physics Laboratory, Johns Hopkins University, Laurel, Maryland, USA, 11NASA Goddard Space Flight Center, observations of the Burns formation: Greenbelt, Maryland, USA, 12Department of Astronomy, Cornell University, Ithaca, New York, USA, 13School of Earth and Crater hopping at Meridiani Planum, J. -
March 21–25, 2016
FORTY-SEVENTH LUNAR AND PLANETARY SCIENCE CONFERENCE PROGRAM OF TECHNICAL SESSIONS MARCH 21–25, 2016 The Woodlands Waterway Marriott Hotel and Convention Center The Woodlands, Texas INSTITUTIONAL SUPPORT Universities Space Research Association Lunar and Planetary Institute National Aeronautics and Space Administration CONFERENCE CO-CHAIRS Stephen Mackwell, Lunar and Planetary Institute Eileen Stansbery, NASA Johnson Space Center PROGRAM COMMITTEE CHAIRS David Draper, NASA Johnson Space Center Walter Kiefer, Lunar and Planetary Institute PROGRAM COMMITTEE P. Doug Archer, NASA Johnson Space Center Nicolas LeCorvec, Lunar and Planetary Institute Katherine Bermingham, University of Maryland Yo Matsubara, Smithsonian Institute Janice Bishop, SETI and NASA Ames Research Center Francis McCubbin, NASA Johnson Space Center Jeremy Boyce, University of California, Los Angeles Andrew Needham, Carnegie Institution of Washington Lisa Danielson, NASA Johnson Space Center Lan-Anh Nguyen, NASA Johnson Space Center Deepak Dhingra, University of Idaho Paul Niles, NASA Johnson Space Center Stephen Elardo, Carnegie Institution of Washington Dorothy Oehler, NASA Johnson Space Center Marc Fries, NASA Johnson Space Center D. Alex Patthoff, Jet Propulsion Laboratory Cyrena Goodrich, Lunar and Planetary Institute Elizabeth Rampe, Aerodyne Industries, Jacobs JETS at John Gruener, NASA Johnson Space Center NASA Johnson Space Center Justin Hagerty, U.S. Geological Survey Carol Raymond, Jet Propulsion Laboratory Lindsay Hays, Jet Propulsion Laboratory Paul Schenk, -
LAYERED SULFATE-BEARING TERRAINS on MARS: INSIGHTS from GALE CRATER and MERIDIANI PLANUM. K.E. Powell1,2, R.E. Arvidson3, and C.S
Ninth International Conference on Mars 2019 (LPI Contrib. No. 2089) 6316.pdf LAYERED SULFATE-BEARING TERRAINS ON MARS: INSIGHTS FROM GALE CRATER AND MERIDIANI PLANUM. K.E. Powell1,2, R.E. Arvidson3, and C.S. Edwards1, 1Department of Physics & Astrono- my, Northern Arizona University, 2School of Earth & Space Exploration, Arizona State University, 3Department of Earth & Planetary Sciences, Washington University in St. Louis. Introduction: Sulfate species have been detected ronment, with episodes of diagenesis and weathering in late Noachian and Hesperian terrains on Mars lying to form a crystalline hematite lag deposit [4, 5]. The stratigraphically above clay minerals, which has been lag deposit masks the CRISM spectral signature of interpreted as documenting a shift from wetter to more sulfate in most locations. Sulfate minerals including arid environments on the surface. Sulfate detections kieserite and gypsum have been detected in impact are associated with layered deposits in numerous loca- crater walls and windswept regions [6]. The Oppor- tions including Gale Crater, Meridiani Planum, Vallis tunity rover explored southern Meridiani Planum Marineris, and Terra Sirenum, and Aram Chaos [1]. through a campaign of crater-hopping, using craters as These sulfates and clays been identified using their a natural drill to expose strata [6]. The deepest expo- diagnostic absorption features in visible and near- sures explored by Opportunity directly are ~10 meters infrared reflectance (VNIR) data acquired from Mars thick at Victoria Crater. Opportunity results indicate orbit. Additionally, two rover missions have explored that the top layers of Burns formation contain up to sites with massive sulfate deposits. The first, the MER 40% sulfate and included Mg, Ca, and Fe species. -
Testable Hypotheses for Opportunity's Traverse
42nd Lunar and Planetary Science Conference (2011) 2199.pdf TESTABLE HYPOTHESES FOR OPPORTUNITY’S TRAVERSE FROM SANTA MARIA TO THE RIM OF ENDEAVOUR CRATER. A. A. Fraeman1, R. E. Arvidson1, S. L. Murchie2, F. P. Seelos2, and J. A. McGo- vern2, 1Washington University in St. Louis, Dept. of Earth and Planetary Science, St. Louis, MO (afrae- [email protected]), 2Johns Hopkins University Applied Physics Laboratory, Laurel, MD Introduction: As of January 2011, the Mars rover Botany Bay and the southern tip of Cape York: Opportunity was located at Santa Maria crater, ~6 km In contrast to the plains, CRISM normal [1] and over- away from the closest rim segment of the ~20 km di- sampled FRT data show signatures of hydrated phases, ameter Noachian-aged impact crater Endeavour (Fig. including hydrated sulfates, present throughout Botany 1). Endeavour predates the sedimentary rocks ex- Bay and the southern point of Cape York (Fig. 3). amined by Opportunity for the past 7 years, and Com- These phases have not been detected from orbit at any pact Reconnaissance Imaging Spectrometer for Mars other location along Opportunity’s ~26km traverse (CRISM) data indicate that Fe-Mg smectites are (with the exception of a small group of CRISM pixels present on the rim of this highly degraded crater [1]. on the SE rim of Santa Maria crater [3]), and suggests The purpose of this abstract is to present working a change in mineralogy occurs, probably at a strati- hypotheses to help guide the acquisition and analysis of graphic contact within Botany Bay. Opportunity’s continued Mars Reconnaissance Orbiter (MRO) cover- ground-truth observations will be essential in determin- age and Opportunity observations as the rover departs ing the nature of these phases as the rover approaches Santa Maria, traverses across the plains, and ascends Cape York, the closest rim segment. -
GRAIL Reveals Secrets of the Lunar Interior
GRAIL Reveals Secrets of the Lunar Interior — Dr. Patrick J. McGovern, Lunar and Planetary Institute A mini-flotilla of spacecraft sent to the Moon in the past few years by several nations has revealed much about the characteristics of the lunar surface via techniques such as imaging, spectroscopy, and laser ranging. While the achievements of these missions have been impressive, only GRAIL has seen deeply enough to reveal inner secrets that the Moon holds. LRecent Lunar Missions Country Name Launch Date Status ESA Small Missions for Advanced September 27, 2003 Ended with lunar surface impact on Research in Technology-1 (SMART-1) September 3, 2006 USA Acceleration, Reconnection, February 27, 2007 Extension of the THEMIS mission; ended Turbulence and Electrodynamics of in 2012 the Moon’s Interaction with the Sun (ARTEMIS) Japan SELENE (Kaguya) September 14, 2007 Ended with lunar surface impact on June 10, 2009 PChina Chang’e-1 October 24, 2007 Taken out of orbit on March 1, 2009 India Chandrayaan-1 October 22, 2008 Two-year mission; ended after 315 days due to malfunction and loss of contact USA Lunar Reconnaissance Orbiter (LRO) June 18, 2009 Completed one-year primary mission; now in five-year extended mission USA Lunar Crater Observation and June 18, 2009 Ended with lunar surface impact on Sensing Satellite (LCROSS) October 9, 2009 China Chang’e-2 October 1, 2010 Primary mission lasted for six months; extended mission completed flyby of asteroid 4179 Toutatis in December 2012 USA Gravity Recovery and Interior September 10, 2011 Ended with lunar surface impact on I Laboratory (GRAIL) December 17, 2012 To probe deeper, NASA launched the Gravity Recovery and Interior Laboratory (GRAIL) mission: twin spacecraft (named “Ebb” and “Flow” by elementary school students from Montana) flying in formation over the lunar surface, tracking each other to within a sensitivity of 50 nanometers per second, or one- twenty-thousandth of the velocity that a snail moves [1], according to GRAIL Principal Investigator Maria Zuber of the Massachusetts Institute of Technology. -
NASA Advisory Council Planetary Protection Subcommittee, May 20‐21, 2014
NASA Advisory Council Planetary Protection Subcommittee, May 20‐21, 2014 NASA ADVISORY COUNCIL Planetary Protection Subcommittee May 20-21, 2014 NASA Headquarters Washington, D.C. MEETING MINUTES _____________________________________________________________ Eugene Levy, Chair ____________________________________________________________ Gale Allen, Executive Secretary Report prepared by Joan M. Zimmermann Zantech IT, Inc. 1 NASA Advisory Council Planetary Protection Subcommittee, May 20-2t 2014 Table of Contents Introduction 3 PPO Update and Review 3 MSL Lessons Learned 5 InSight Status 8 Planetary Science and Mars Program Update 10 Contamination Limits for Planetary Life Detection 12 Mars Landing Site Selection Process 14 ESA 2018 Landing Site Selection 15 Mars 2020 Project Status 15 Public Comment 16 Discussion 16 Ethics Briefing 17 Discussion 17 Science Mission Directorate and Planetary Protection 17 Update on Special Regions Parameters 19 Status of Phobos /Demos Materials 21 Outer Solar System Special Regions: Enceladus and Beyond 22 JAXA Sample Return Working Group 23 Public Comment 24 Discussion 25 Appendix A- Attendees Appendix 8- Membership roster Appendix C- Presentations Appendix D- Agenda 2 NASA Advisory Council Planetary Protection Subcommittee, May 20-2t 2014 May 20.2014 Introduction The Executive Secretary of the Planetary Protection Subcommittee (PPS), Dr. Gale Allen, made preparatory announcements. Dr. Eugene Levy, PPS Chair, opened the meeting and noted there would be a heavy focus on Mars exploration, as it has become a timely and important issue. Introductions were made around the meeting room. Planetary Protection Office Update and Review Dr. Catharine Conley, Planetary Protection Officer (PPO) for NASA, briefly described the broad base of experience in the PPS, and reviewed the purpose of Planetary Protection (PP) and the policy, as it applies to all missions. -
Terrestrial Planets 1- 4 from the Sun Mercury in Sight
Terrestrial Planets 1- 4 from the Sun Image courtesy: http://commons.wikimedia.org/wiki/Image:Terrestrial_planet_size_comparisons_edit.jpg First ever ‘whole Earth’ picture from deep space, taken by Bill Anders on Apollo 8 Apollo 8 crew, Bill Anders centre: courtesy Nasa Mercury, Venus, Earth and Mars are four The Earth is just a planet astonishingly different planets Mercury and Venus have only been seen in any detail within the last 30 years Mercury in sight Mercury Mercury is like the Earth inside and the Moon outside Courtesy NASA (Mariner 10) Mercury has had a cooling and bombardment history Mercury is visible only soon after the setting similar to the moon sun or shortly before dawn It appears as cratered lava the Mariner 10 probe (1974/75) is the source of most information about Mercury – Messenger, launched 2004, with scarps first flypast in 2008 and orbit Mercury in 2011. ESA’s Its rocks are Earth-like BepiColombo, to be launched in 2013 Mariner 10 image Messenger images Messenger image ↑ Double-ringed crater – a Mercury feature courtesy: http://messenger.jhuapl.edu/gallery/sciencePhotos/pics/S trom02.jpg ← Courtesy: http://messenger.jhuapl.edu/gal lery/sciencePhotos/pics/EN010 8828161M.jpg Courtesy: http://messenger.jhuapl.edu/gallery/sciencePhotos/pics/Prockter06.jpg Messenger image Mercury Close-up Mercury’s topography was formed under stronger The gravity than on the Moon caloris The Caloris basin is an impact crater ~1400 km across, basin is the beneath which is thought to be a dense mass large 2 Mercury’s rotation period is exactly /3 of its orbital circular period of 87.97 days. -
14Yearsofdiscovery
14 YEARS OF DISCOVERIES 14 years of discoveries 14 YEARS OF DISCOVERIES DesignedMARS to last 90 days, Opportunity survived for over a 1 Martian solar decade on Mars. Here day (Sol) we look back on how = the record-breaking 1.027 rover changed the way Earth days we see the Red Planet 2 14 years of discoveries 39 Sols 91 Sols Opportunity’s Opportunity from orbit Opportunity’s journey across Mars has objectives been closely watched and calibrated by the satellites in orbit around the Red Search for signs of past Planet. This image from NASA’s Mars ✔ Global Surveyor shows some of the liquid water tracks of the rover, the craters it was visiting, its back shell and parachute, Determine distribution along with the location of its discarded and composition of heat shield. It was taken on 26 April Martian rocks ✔ 2004 on Sol 91 from a distance of around 400 kilometres (249 miles). Discover the geological processes which formed the Martian terrain ✔ Validate measurements made by probes orbiting Mars ✔ Search for iron containing minerals that may have been formed in water ✔ Signs of past water This is a microscopic image of part of a rock called 'Last Determine the texture of Chance'. The view here is around five centimetres (two rocks and soils and what inches) across and was taken on Opportunity’s 39th created them ✔ Martian day. The texture of the rock has led scientists to believe that water was once present in the area in which Assess whether Mars’ climate it was found – the Meridiani Planum area of Mars, which was ever fit for life ✔ is close to its equator.