DOCSLIB.ORG

Future Mars Geophysical Observatories for Understanding Its Internal Structure, Rotation, and Evolution

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text
Future Mars Geophysical Observatories for Understanding Its Internal Structure, Rotation, and Evolution Planetary and Space Science 68 (2012) 123–145 Contents lists available at SciVerse ScienceDirect Planetary and Space Science journal homepage: www.elsevier.com/locate/pss Future Mars geophysical observatories for understanding its internal structure, rotation, and evolution Veronique Dehant a,n, Bruce Banerdt b, Philippe Lognonne´ c, Matthias Grott d, Sami Asmar b, Jens Biele e, Doris Breuer d, Franc-ois Forget f, Ralf Jaumann d, Catherine Johnson g,h, Martin Knapmeyer d, Benoit Langlais i, Mathieu Le Feuvre i, David Mimoun j, Antoine Mocquet i, Peter Read k, Attilio Rivoldini a,l, Oliver Romberg m, Gerald Schubert n, Sue Smrekar b, Tilman Spohn d, Paolo Tortora o, Stephan Ulamec e, Susanne Vennerstrøm p a Royal Observatory of Belgium, Belgium b Jet Propulsion Laboratory, USA c Institut de Physique du Globe, Sorbonne Paris Cite´, Univ. Paris Diderot, France d Institute of Planetary Research, DLR, Germany e German Space Operations Center/GSOC, DLR, Germany f Laboratoire de Me´te´orologie Dynamique, Paris, France g Department of Earth and Ocean Sciences, University of British Columbia, Vancouver, Canada h Planetary Science Institute, Tucson, USA i Laboratoire de Plane´tologie et Ge´odynamique, UMR 6112, Universite´ de Nantes, Nantes Atlantique Universite´s, CNRS, France j Universite´ de Toulouse, ISAE/Supaero, Toulouse, France k Atmospheric Oceanic and Planetary Physics, Oxford Physics, UK l Universite´ catholique de Louvain, Earth and Life Institute (ELI), Georges Lemaˆıtre Centre for Earth and Climate Research (TECLIM), Belgium m Institute of Space Systems (DLR), Bremen, Germany n University of California, Los Angeles, USA o University of Bologna, Italy p National Space Institute, Technical University of Denmark, Denmark article info abstract Article history: Our fundamental understanding of the interior of the Earth comes from seismology, geodesy, Received 20 February 2011 geochemistry, geomagnetism, geothermal studies, and petrology. For the Earth, measurements in those Received in revised form disciplines of geophysics have revealed the basic internal layering of the Earth, its dynamical regime, its 26 October 2011 thermal structure, its gross compositional stratification, as well as significant lateral variations in these Accepted 29 October 2011 quantities. Planetary interiors not only record evidence of conditions of planetary accretion and Available online 26 November 2011 differentiation, they exert significant control on surface environments. Keywords: We present recent advances in possible in-situ investigations of the interior of Mars, experiments Interior structure and strategies that can provide unique and critical information about the fundamental processes of Rotation terrestrial planet formation and evolution. Such investigations applied on Mars have been ranked as a Magnetic field high priority in virtually every set of European, US and international high-level planetary science Heat flow Seismology recommendations for the past 30 years. New seismological methods and approaches based on the Mars cross-correlation of seismic noise by two seismic stations/landers on the surface of Mars and on joint Atmosphere seismic/orbiter detection of meteorite impacts, as well as the improvement of the performance of Very Habitability Broad-Band (VBB) seismometers have made it possible to secure a rich scientific return with only two simultaneously recording stations. In parallel, use of interferometric methods based on two Earth–Mars radio links simultaneously from landers tracked from Earth has increased the precision of radio science experiments by one order of magnitude. Magnetometer and heat flow measurements will complement seismic and geodetic data in order to obtain the best information on the interior of Mars. n Corresponding author. Tel.: þ322 373 0266; fax: þ322 374 9822. E-mail addresses: [email protected], [email protected] (V. Dehant), [email protected] (B. Banerdt), [email protected] (P. Lognonne´), [email protected] (M. Grott), [email protected] (S. Asmar), [email protected] (J. Biele), [email protected] (D. Breuer), [email protected] (F. Forget), [email protected] (R. Jaumann), [email protected] (C. Johnson), [email protected] (M. Knapmeyer), [email protected] (B. Langlais), [email protected] (M. Le Feuvre), [email protected] (D. Mimoun), [email protected] (A. Mocquet), [email protected] (P. Read), [email protected] (A. Rivoldini), [email protected] (O. Romberg), [email protected] (G. Schubert), [email protected] (S. Smrekar), [email protected] (T. Spohn), [email protected] (P. Tortora), [email protected] (S. Ulamec), [email protected] (S. Vennerstrøm). 0032-0633/$ - see front matter & 2011 Elsevier Ltd. All rights reserved. doi:10.1016/j.pss.2011.10.016 124 V. Dehant et al. / Planetary and Space Science 68 (2012) 123–145 In addition to studying the present structure and dynamics of Mars, these measurements will provide important constraints for the astrobiology of Mars by helping to understand why Mars failed to sustain a magnetic field, by helping to understand the planet’s climate evolution, and by providing a limit for the energy available to the chemoautotrophic biosphere through a measurement of the surface heat flow. The landers of the mission will also provide meteorological stations to monitor the climate and obtain new measurements in the atmospheric boundary layer. & 2011 Elsevier Ltd. All rights reserved. 1. Introduction et al., 2006) and more recently to the determination of the core size and state with tidal measurement (Williams et al., 1996, 1.1. Why study Mars? 2001) and modern seismic processing (Weber et al., 2011; Garcia et al., 2011). Subsequently, with the development of seismic By studying other planets, we seek to understand the pro- networks on the Earth, seismology has mapped the structure of cesses that govern planetary evolution and discover the factors core–mantle boundary, density and phase changes in the mantle, that have led to the unique evolution of Earth. Why is Earth the three-dimensional velocity anomalies in the mantle related to only planet with surface liquid oceans, plate tectonics, and sub-solidus convection, and lateral variations in lithospheric abundant life? Mars is presently on the edge of the habitable structure. Additionally, seismic information places constraints zone, but may have been much more hospitable early in its on Earth’s interior temperature distribution and on the boundary history. Recent surveys of Mars suggest that the formation of conditions at the top and bottom of the outer core, which govern rocks in the presence of abundant water was largely confined to the mechanisms of geodynamo operation (e.g., Aubert et al., the earliest geologic epoch, the Noachian age (prior to 3.8 Ga) 2008). Thus physical properties inferred from seismic data are used (Poulet et al., 2005). This early period of Martian history was in almost any modeling of the Earth’s thermal and volatile evolution, extremely dynamic, witnessing planetary differentiation, forma- including the exchange of volatiles among different reservoirs tion of the core, an active dynamo, the formation of the bulk of (McGovern and Schubert, 1989; van Keken and Ballentine, 1999; the crust and the establishment of the major geologic divisions Franck and Bounama, 1997, 2000; Schubert et al., 2001; Guest and (Solomon et al., 2005). Formation of the crust and associated Smrekar, 2007; Smrekar and Guest, 2007), and their impact on the volcanism released volatiles from the interior into the atmo- long term habitability of the planet. sphere (Greeley, 1987; Phillips et al., 2001; Gillmann et al., 2009), The main difference between the Earth and Mars is that the causing conditions responsible for the formation of the familiar latter still preserves many billion year old crustal and potentially signs of liquid water on the surface of Mars, from the abundant mantle structures on a planetary spatial scale (e.g., the heavily channels, phyllosilicate formations and carbonate deposits to cratered southern hemisphere of Mars), while the ocean floor that sulfate-rich layered outcrops (Poulet et al., 2005; Clark et al., covers about two-thirds of the Earth’s surface is younger than 250 2005; Bridges et al., 2001; Ehlmann et al., 2008; Morris et al., million years, due to plate tectonics and associated recycling of 2010). the Earth’s lithosphere. Martian meteorite compositions indicate melting source regions with different compositions that have 1.2. Why study the geophysics of Mars? persisted since the earliest evolution of the planet (Jones, 1986; Borg et al., 1997, 2002). Further, much of the Martian crust dates Studying the geophysics of Mars, focusing on interior pro- to the first half billion years of solar system history (Frey et al., cesses and early evolution, provides essential constraints for 2002; Frey, 2006a, 2006b). Measurements of the interior are likely models of the thermal, geochemical, and geologic evolution of to detect mantle inhomogeneities that still reflect differentiation Mars and for the correct use of the constraints from SNC and early planetary formation processes, making Mars an ideal meteorites (considered to be Martian rocks, based on a close subject for geophysical investigations aimed at understanding match between the composition of gases included and the atmo- planetary accretion and early evolution. sphere of Mars, often used in the literature to constrain the Subsequent to initial differentiation, Mars and the Earth Martian mantle composition; e.g., Wanke¨ and Dreibus, 1988; diverged in their evolution. Earth’s thermal engine has transferred Hauck and Phillips, 2002) and any future samples from Mars. heat to the surface largely by lithospheric recycling over much of Our fundamental understanding of the interior of the Earth its history, but on Mars there is no evidence in the available (and of the Moon) comes from geophysics, geodesy, geochemis- record that this process ever occurred (e.g., Pruis and Tanaka, try, and petrology. For geophysics, seismology, geodesy, and heat 1995; Sleep and Tanaka, 1995).
Load more

Recommended publications
  • Owner's Manual,1996 Pontiac Bonneville
    I LLt -The 1996 Pontiac Bonneville Owner’s Manual Seats and Restraint Systems ............................................................. 1-1 This section tells you how to use your seats and safety belts properly. It also explains“SRS” the system. Features and Controls ..................... ;............................................ 2-1 This section explainshow to start and operate your Pontiac. Comfort Controls and Audio Systems ...................................................... 3-1 This section tells you how to adjust the ventilation and comfort controls andhow to operate your audio system. Your Driving and the Road .............................................................. 4-1 Here you’ll find helpful information and tips about the roadhow and to drive under different conditions. ProblemsontheRoad .................................................................. 5-1 This section tells you whatto do if you have a problem whiledriving, such as a flat tire or overheated engine, etc. Service and Appearance Care.. .......................................................... 6-1 Here the manual tellsyou how to keep your Pontiacrunning properly and looking good. Maintenanceschedule......... .......................................................... 7-1 This section tellp you when to perform vehicle maintenance and what fluidsand lubricants to use. Customer Assistance Information ... .#.................................................... 8-1 \ This section tells youhow to contact Pontiac for assistance and how to get service and
    [Show full text]
  • NASA's Lunar Atmosphere and Dust Environment Explorer (LADEE)
    Geophysical Research Abstracts Vol. 13, EGU2011-5107-2, 2011 EGU General Assembly 2011 © Author(s) 2011 NASA’s Lunar Atmosphere and Dust Environment Explorer (LADEE) Richard Elphic (1), Gregory Delory (1,2), Anthony Colaprete (1), Mihaly Horanyi (3), Paul Mahaffy (4), Butler Hine (1), Steven McClard (5), Joan Salute (6), Edwin Grayzeck (6), and Don Boroson (7) (1) NASA Ames Research Center, Moffett Field, CA USA ([email protected]), (2) Space Sciences Laboratory, University of California, Berkeley, CA USA, (3) Laboratory for Atmospheric and Space Physics, University of Colorado, Boulder, CO USA, (4) NASA Goddard Space Flight Center, Greenbelt, MD USA, (5) LunarQuest Program Office, NASA Marshall Space Flight Center, Huntsville, AL USA, (6) Planetary Science Division, Science Mission Directorate, NASA, Washington, DC USA, (7) Lincoln Laboratory, Massachusetts Institute of Technology, Lexington MA USA Nearly 40 years have passed since the last Apollo missions investigated the mysteries of the lunar atmosphere and the question of levitated lunar dust. The most important questions remain: what is the composition, structure and variability of the tenuous lunar exosphere? What are its origins, transport mechanisms, and loss processes? Is lofted lunar dust the cause of the horizon glow observed by the Surveyor missions and Apollo astronauts? How does such levitated dust arise and move, what is its density, and what is its ultimate fate? The US National Academy of Sciences/National Research Council decadal surveys and the recent “Scientific Context for Exploration of the Moon” (SCEM) reports have identified studies of the pristine state of the lunar atmosphere and dust environment as among the leading priorities for future lunar science missions.
    [Show full text]
  • Hip # 987-1088
    Hip No. Consigned by Tate Farms Hip No. 987 Jess Sizzlin SI 92 987 1997 Sorrel Mare Streakin La Jolla SI 99 {Streakin Six SI 104 Mr Jess Perry SI 113 { Bottom’s Up SI 82 Scoopie Fein SI 99 {Sinn Fein SI 98 Jess Sizzlin SI 92 Legs La Scoop SI 95 3654393 Easy Jet SI 100 {Jet Deck SI 100 Sizzlin Kim SI 86 Lena’s Bar TB SI 95 (1987) { Sun Spots {Double Bid SI 100 Winsum Miss SI 95 By MR JESS PERRY SI 113 (1992). Champion 2-year-old, $687,184 [G1]. Sire of 799 ROM, 107 stakes winners, $39,619,142, incl. champions APOL- LITICAL JESS SI 107 (world champion, $1,399,831, Los Alamitos Derby [G1]), ONE FAMOUS EAGLE SI 101 ($1,387,453 [G1]). Sire of the dams of 46 stakes winners, incl. BODACIOUS DASH SI 101 ($756,495 [G1]), JES A GAME SI 111 ($323,978 [G2]), TERRIFIC SYNERGY SI 92 ($288,066 [RG2]). 1st dam SIZZLIN KIM SI 86, by Easy Jet. Placed to 3. Dam of 7 foals, 6 to race, 3 winners, including– Jess Sizzlin SI 92 (f. by Mr Jess Perry). Stakes placed winner, below. Streakin Kim (f. by Streakin La Jolla). Unplaced. Dam of– Kims Corona SI 97 (g. by Corona Cocktail). 3 wins to 4, $38,666. 2nd dam SUN SPOTS, by Double Bid. Unraced. Dam of 13 starters, 7 ROM, incl.– SUN KISSES SI 102 (f. by Game Plan). 7 wins to 3, $68,935, Shebester Derby, Mystery Derby. Dam of Exquisite Expense SI 99 ($42,264 [G3]).
    [Show full text]
  • Widespread Crater-Related Pitted Materials on Mars: Further Evidence for the Role of Target Volatiles During the Impact Process ⇑ Livio L
    Icarus 220 (2012) 348–368 Contents lists available at SciVerse ScienceDirect Icarus journal homepage: www.elsevier.com/locate/icarus Widespread crater-related pitted materials on Mars: Further evidence for the role of target volatiles during the impact process ⇑ Livio L. Tornabene a, , Gordon R. Osinski a, Alfred S. McEwen b, Joseph M. Boyce c, Veronica J. Bray b, Christy M. Caudill b, John A. Grant d, Christopher W. Hamilton e, Sarah Mattson b, Peter J. Mouginis-Mark c a University of Western Ontario, Centre for Planetary Science and Exploration, Earth Sciences, London, ON, Canada N6A 5B7 b University of Arizona, Lunar and Planetary Lab, Tucson, AZ 85721-0092, USA c University of Hawai’i, Hawai’i Institute of Geophysics and Planetology, Ma¯noa, HI 96822, USA d Smithsonian Institution, Center for Earth and Planetary Studies, Washington, DC 20013-7012, USA e NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA article info abstract Article history: Recently acquired high-resolution images of martian impact craters provide further evidence for the Received 28 August 2011 interaction between subsurface volatiles and the impact cratering process. A densely pitted crater-related Revised 29 April 2012 unit has been identified in images of 204 craters from the Mars Reconnaissance Orbiter. This sample of Accepted 9 May 2012 craters are nearly equally distributed between the two hemispheres, spanning from 53°Sto62°N latitude. Available online 24 May 2012 They range in diameter from 1 to 150 km, and are found at elevations between À5.5 to +5.2 km relative to the martian datum. The pits are polygonal to quasi-circular depressions that often occur in dense clus- Keywords: ters and range in size from 10 m to as large as 3 km.
    [Show full text]
  • Geologic Map of the Twin Falls 30 X 60 Minute Quadrangle, Idaho
    Geologic Map of the Twin Falls 30 x 60 Minute Quadrangle, Idaho Compiled and Mapped by Kurt L. Othberg, John D. Kauffman, Virginia S. Gillerman, and Dean L. Garwood 2012 Idaho Geological Survey Third Floor, Morrill Hall University of Idaho Geologic Map 49 Moscow, Idaho 83843-3014 2012 Geologic Map of the Twin Falls 30 x 60 Minute Quadrangle, Idaho Compiled and Mapped by Kurt L. Othberg, John D. Kauffman, Virginia S. Gillerman, and Dean L. Garwood INTRODUCTION 43˚ 115˚ The geology in the 1:100,000-scale Twin Falls 30 x 23 13 18 7 8 25 60 minute quadrangle is based on field work conduct- ed by the authors from 2002 through 2005, previous 24 17 14 16 19 20 26 1:24,000-scale maps published by the Idaho Geological Survey, mapping by other researchers, and compilation 11 10 from previous work. Mapping sources are identified 9 15 12 6 in Figures 1 and 2. The geologic mapping was funded in part by the STATEMAP and EDMAP components 5 1 2 22 21 of the U.S. Geological Survey’s National Cooperative 4 3 42˚ 30' Geologic Mapping Program (Figure 1). We recognize 114˚ that small map units in the Snake River Canyon are dif- 1. Bonnichsen and Godchaux, 1995a 15. Kauffman and Othberg, 2005a ficult to identify at this map scale and we direct readers 2. Bonnichsen and Godchaux, 16. Kauffman and Othberg, 2005b to the 1:24,000-scale geologic maps shown in Figure 1. 1995b; Othberg and others, 2005 17. Kauffman and others, 2005a 3.
    [Show full text]
  • Crater Geometry and Ejecta Thickness of the Martian Impact Crater Tooting
    Meteoritics & Planetary Science 42, Nr 9, 1615–1625 (2007) Abstract available online at http://meteoritics.org Crater geometry and ejecta thickness of the Martian impact crater Tooting Peter J. MOUGINIS-MARK and Harold GARBEIL Hawai‘i Institute of Geophysics and Planetology, University of Hawai‘i, Honolulu, Hawai‘i 96822, USA (Received 25 October 2006; revision accepted 04 March 2007) Abstract–We use Mars Orbiter Laser Altimeter (MOLA) topographic data and Thermal Emission Imaging System (THEMIS) visible (VIS) images to study the cavity and the ejecta blanket of a very fresh Martian impact crater ~29 km in diameter, with the provisional International Astronomical Union (IAU) name Tooting crater. This crater is very young, as demonstrated by the large depth/ diameter ratio (0.065), impact melt preserved on the walls and floor, an extensive secondary crater field, and only 13 superposed impact craters (all 54 to 234 meters in diameter) on the ~8120 km2 ejecta blanket. Because the pre-impact terrain was essentially flat, we can measure the volume of the crater cavity and ejecta deposits. Tooting crater has a rim height that has >500 m variation around the rim crest and a very large central peak (1052 m high and >9 km wide). Crater cavity volume (i.e., volume below the pre-impact terrain) is ~380 km3 and the volume of materials above the pre-impact terrain is ~425 km3. The ejecta thickness is often very thin (<20 m) throughout much of the ejecta blanket. There is a pronounced asymmetry in the ejecta blanket, suggestive of an oblique impact, which has resulted in up to ~100 m of additional ejecta thickness being deposited down-range compared to the up-range value at the same radial distance from the rim crest.
    [Show full text]
  • Obituaries, A
    OBITUARIES, A - K Updated 7/31/2020 Bernardsville Library Local History Room NAME TITLE DATE OF DEATH SOURCE EDITION PAGE AGE NOTES NJ Archives Abstract & Aaron, Robert 01/13/1802 Wills Vol.X 1801-1805 7 Abantanzo, Marie 01/13/1923 Bernardsville News 01/18/1923 4 Abbate, Michael 06/22/1955 Bernardsville News 06/23/1955 1 Abberman, Jay 04/10/2005 Bernardsville News 04/14/2005 10 82 Abbey, E. Mrs. 06/02/1957 Bernardsville News 06/06/1957 4 Abbond, Doris Weakley 03/27/2000 Bernardsville News 03/30/2000 10 80 Abbond, Robert R. 02/09/1995 Bernardsville News 02/15/1995 10 82 Abbondanzo, Delores L. 11/03/2001 Bernardsville News 11/08/2001 11 75 Abbondanzo, Francis J. 12/26/1993 Bernardsville News 12/29/1993 10 69 Abbondanzo, L. Mrs. 12/22/1962 Bernardsville News 01/03/1963 2 Abbondanzo, Lena I. 05/08/2003 Bernardsville News 05/15/2003 10 80 Abbondanzo, Louis 12/23/1979 Bernardsville News 01/03/1980 6 89 Abbondanzo, Louis J. 12/25/1993 Bernardsville News 12/29/1993 10 65 Abbondanzo, Mary G. 06/12/2014 Bernardsville News 06/26/2014 8 88 Abbondanzo, Patricia A. 11/21/1983 Bernardsville News 11/24/1983 Abbondanzo, Patrick J. 12/11/2000 Bernardsville News 12/14/2000 10 78 Abbondanzo, Rose 12/22/1962 Bernardsville News 01/03/1963 2 63 Abbondanzo, Sharon J. 08/28/2013 Bernardsville News 09/05/2013 9 78 Abbondanzo, Vincent J. 07/26/1996 Bernardsville News 07/31/1996 10 66 Abbott, Charles Cortez Jr.
    [Show full text]
  • Mars Science Laboratory Entry Capsule Aerothermodynamics and Thermal Protection System
    Mars Science Laboratory Entry Capsule Aerothermodynamics and Thermal Protection System Karl T. Edquist ([email protected], 757-864-4566) Brian R. Hollis ([email protected], 757-864-5247) NASA Langley Research Center, Hampton, VA 23681 Artem A. Dyakonov ([email protected], 757-864-4121) National Institute of Aerospace, Hampton, VA 23666 Bernard Laub ([email protected], 650-604-5017) Michael J. Wright ([email protected], 650-604-4210) NASA Ames Research Center, Moffett Field, CA 94035 Tomasso P. Rivellini ([email protected], 818-354-5919) Eric M. Slimko ([email protected], 818-354-5940) Jet Propulsion Laboratory, Pasadena, CA 91109 William H. Willcockson ([email protected], 303-977-5094) Lockheed Martin Space Systems Company, Littleton, CO 80125 Abstract—The Mars Science Laboratory (MSL) spacecraft TABLE OF CONTENTS is being designed to carry a large rover (> 800 kg) to the 1. INTRODUCTION ..................................................... 1 surface of Mars using a blunt-body entry capsule as the 2. COMPUTATIONAL RESULTS ................................. 2 primary decelerator. The spacecraft is being designed for 3. EXPERIMENTAL RESULTS .................................... 5 launch in 2009 and arrival at Mars in 2010. The 4. TPS TESTING AND MODEL DEVELOPMENT.......... 7 combination of large mass and diameter with non-zero 5. SUMMARY ........................................................... 11 angle-of-attack for MSL will result in unprecedented REFERENCES........................................................... 11 convective heating environments caused by turbulence prior BIOGRAPHY ............................................................ 12 to peak heating. Navier-Stokes computations predict a large turbulent heating augmentation for which there are no supporting flight data1 and little ground data for validation.
    [Show full text]
  • Carbon Monoxide As a Metabolic Energy Source for Extremely Halophilic Microbes: Implications for Microbial Activity in Mars Regolith
    Carbon monoxide as a metabolic energy source for extremely halophilic microbes: Implications for microbial activity in Mars regolith Gary M. King1 Department of Biological Sciences, Louisiana State University, Baton Rouge, LA 70803 Edited by David M. Karl, University of Hawaii, Honolulu, HI, and approved March 5, 2015 (received for review December 31, 2014) Carbon monoxide occurs at relatively high concentrations (≥800 that low organic matter levels might indeed occur in some deposits parts per million) in Mars’ atmosphere, where it represents a poten- (e.g., 12). Even so, it is uncertain whether this material exists in a tially significant energy source that could fuel metabolism by a local- form or concentrations suitable for microbial use. ized putative surface or near-surface microbiota. However, the The Martian atmosphere has largely been ignored as a potential plausibility of CO oxidation under conditions relevant for Mars in energy source, because it is dominated by CO2 (24, 25). Ironically, its past or at present has not been evaluated. Results from diverse UV photolysis of CO2 forms carbon monoxide (CO), a potential terrestrial brines and saline soils provide the first documentation, to bacterial substrate that occurs at relatively high concentrations: our knowledge, of active CO uptake at water potentials (−41 MPa to about 800 ppm on average, with significantly higher levels for −117 MPa) that might occur in putative brines at recurrent slope some sites and times (26, 27). In addition, molecular oxygen lineae (RSL) on Mars. Results from two extremely halophilic iso- (O2), which can serve as a biological CO oxidant, occurs at lates complement the field observations.
    [Show full text]
  • First Year of Coordinated Science Observations by Mars Express and Exomars 2016 Trace Gas Orbiter
    MANUSCRIPT PRE-PRINT Icarus Special Issue “From Mars Express to ExoMars” https://doi.org/10.1016/j.icarus.2020.113707 First year of coordinated science observations by Mars Express and ExoMars 2016 Trace Gas Orbiter A. Cardesín-Moinelo1, B. Geiger1, G. Lacombe2, B. Ristic3, M. Costa1, D. Titov4, H. Svedhem4, J. Marín-Yaseli1, D. Merritt1, P. Martin1, M.A. López-Valverde5, P. Wolkenberg6, B. Gondet7 and Mars Express and ExoMars 2016 Science Ground Segment teams 1 European Space Astronomy Centre, Madrid, Spain 2 Laboratoire Atmosphères, Milieux, Observations Spatiales, Guyancourt, France 3 Royal Belgian Institute for Space Aeronomy, Brussels, Belgium 4 European Space Research and Technology Centre, Noordwijk, The Netherlands 5 Instituto de Astrofísica de Andalucía, Granada, Spain 6 Istituto Nazionale Astrofisica, Roma, Italy 7 Institut d'Astrophysique Spatiale, Orsay, Paris, France Abstract Two spacecraft launched and operated by the European Space Agency are currently performing observations in Mars orbit. For more than 15 years Mars Express has been conducting global surveys of the surface, the atmosphere and the plasma environment of the Red Planet. The Trace Gas Orbiter, the first element of the ExoMars programme, began its science phase in 2018 focusing on investigations of the atmospheric composition with unprecedented sensitivity as well as surface and subsurface studies. The coordination of observation programmes of both spacecraft aims at cross calibration of the instruments and exploitation of new opportunities provided by the presence of two spacecraft whose science operations are performed by two closely collaborating teams at the European Space Astronomy Centre (ESAC). In this paper we describe the first combined observations executed by the Mars Express and Trace Gas Orbiter missions since the start of the TGO operational phase in April 2018 until June 2019.
    [Show full text]
  • Insight Spacecraft Launch for Mission to Interior of Mars
    InSight Spacecraft Launch for Mission to Interior of Mars InSight is a robotic scientific explorer to investigate the deep interior of Mars set to launch May 5, 2018. It is scheduled to land on Mars November 26, 2018. It will allow us to better understand the origin of Mars. First Launch of Project Orion Project Orion took its first unmanned mission Exploration flight Test-1 (EFT-1) on December 5, 2014. It made two orbits in four hours before splashing down in the Pacific. The flight tested many subsystems, including its heat shield, electronics and parachutes. Orion will play an important role in NASA's journey to Mars. Orion will eventually carry astronauts to an asteroid and to Mars on the Space Launch System. Mars Rover Curiosity Lands After a nine month trip, Curiosity landed on August 6, 2012. The rover carries the biggest, most advanced suite of instruments for scientific studies ever sent to the martian surface. Curiosity analyzes samples scooped from the soil and drilled from rocks to record of the planet's climate and geology. Mars Reconnaissance Orbiter Begins Mission at Mars NASA's Mars Reconnaissance Orbiter launched from Cape Canaveral August 12. 2005, to find evidence that water persisted on the surface of Mars. The instruments zoom in for photography of the Martian surface, analyze minerals, look for subsurface water, trace how much dust and water are distributed in the atmosphere, and monitor daily global weather. Spirit and Opportunity Land on Mars January 2004, NASA landed two Mars Exploration Rovers, Spirit and Opportunity, on opposite sides of Mars.
    [Show full text]
  • Maven by Example I
    Maven by Example i Maven by Example Ed. 0.7 Maven by Example ii Contents 1 Introducing Apache Maven1 1.1 Maven. What is it?....................................1 1.2 Convention Over Configuration...............................2 1.3 A Common Interface....................................3 1.4 Universal Reuse through Maven Plugins..........................3 1.5 Conceptual Model of a “Project”..............................4 1.6 Is Maven an alternative to XYZ?..............................5 1.7 Comparing Maven with Ant................................6 2 Installing Maven 10 2.1 Verify your Java Installation................................ 10 2.2 Downloading Maven.................................... 11 2.3 Installing Maven...................................... 11 Maven by Example iii 2.3.1 Installing Maven on Linux, BSD and Mac OS X................. 11 2.3.2 Installing Maven on Microsoft Windows...................... 12 2.3.2.1 Setting Environment Variables..................... 12 2.4 Testing a Maven Installation................................ 13 2.5 Maven Installation Details................................. 13 2.5.1 User-Specific Configuration and Repository.................... 14 2.5.2 Upgrading a Maven Installation.......................... 15 2.6 Uninstalling Maven..................................... 15 2.7 Getting Help with Maven.................................. 15 2.8 About the Apache Software License............................ 16 3 A Simple Maven Project 17 3.1 Introduction......................................... 17 3.1.1 Downloading
    [Show full text]