Science of Subsurface Habitability & Life on Mars
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DID MARS EVER HAVE a LIVELY UNDERGROUND SCENE? Joseph
Third Conference on Early Mars (2012) 7060.pdf DID MARS EVER HAVE A LIVELY UNDERGROUND SCENE? Joseph. R. Michalski, Natural History Mu- seum, London, UK and Planetary Science Institute, Tucson, AZ, USA. [email protected] Introduction: Prokaryotes comprise more than are investigating environments that might never have 50% of the Earth’s organic carbon, and the amount of been inhabited on a planet that is very much habitable. prokaryote biomass in the deep subsurface is 10-15 Spectroscopic results over the last 5-10 years have times the combined mass of prokaryotes that inhabit revealed significant diversity, abundance, and distribu- the oceans and terrestrial surface combined [1]. We do tion of alteration minerals that formed from aqueous not know when the first life occurred on Earth, but the processes on ancient Mars (recently summarized by first evidence is found in some of the oldest preserved Ehlmann et al. [6]). The mineralogy and context of rocks dating to 3.5 or, as much as 3.8 Ga [2]. While the these altered deposits indicates that deep hydrothermal concept of a “tree of life” breaks down in the Archean processes have operated on Mars, and might have per- [3], it seems likely that the most primitive ancestors of sisted from the Noachian into the Hesperian or later. In all life on Earth correspond to thermophile this work, I consider the implications of recent results chemoautotrophs. Perhaps these are the only life forms for the habitability of the subsurface, the occurrence of that survived intense heat flow during the Late Heavy groundwater, and the possibility to access materials Bombardment or perhaps they actually represent the representing subsurface biological processes. -
Westminsterresearch the Astrobiology Primer V2.0 Domagal-Goldman, S.D., Wright, K.E., Adamala, K., De La Rubia Leigh, A., Bond
WestminsterResearch http://www.westminster.ac.uk/westminsterresearch The Astrobiology Primer v2.0 Domagal-Goldman, S.D., Wright, K.E., Adamala, K., de la Rubia Leigh, A., Bond, J., Dartnell, L., Goldman, A.D., Lynch, K., Naud, M.-E., Paulino-Lima, I.G., Kelsi, S., Walter-Antonio, M., Abrevaya, X.C., Anderson, R., Arney, G., Atri, D., Azúa-Bustos, A., Bowman, J.S., Brazelton, W.J., Brennecka, G.A., Carns, R., Chopra, A., Colangelo-Lillis, J., Crockett, C.J., DeMarines, J., Frank, E.A., Frantz, C., de la Fuente, E., Galante, D., Glass, J., Gleeson, D., Glein, C.R., Goldblatt, C., Horak, R., Horodyskyj, L., Kaçar, B., Kereszturi, A., Knowles, E., Mayeur, P., McGlynn, S., Miguel, Y., Montgomery, M., Neish, C., Noack, L., Rugheimer, S., Stüeken, E.E., Tamez-Hidalgo, P., Walker, S.I. and Wong, T. This is a copy of the final version of an article published in Astrobiology. August 2016, 16(8): 561-653. doi:10.1089/ast.2015.1460. It is available from the publisher at: https://doi.org/10.1089/ast.2015.1460 © Shawn D. Domagal-Goldman and Katherine E. Wright, et al., 2016; Published by Mary Ann Liebert, Inc. This Open Access article is distributed under the terms of the Creative Commons Attribution Noncommercial License (http://creativecommons.org/licenses/by- nc/4.0/) which permits any noncommercial use, distribution, and reproduction in any medium, provided the original author(s) and the source are credited. The WestminsterResearch online digital archive at the University of Westminster aims to make the research output of the University available to a wider audience. -
SPORADIC GROUNDWATER UPWELLING in DEEP MARTIAN CRATERS: EVIDENCE for LACUSTRINE CLAYS and CARBONATES. J. R. Michalski1,2, A. D. Rogers3, S
SPORADIC GROUNDWATER UPWELLING IN DEEP MARTIAN CRATERS: EVIDENCE FOR LACUSTRINE CLAYS AND CARBONATES. J. R. Michalski1,2, A. D. Rogers3, S. P. Wright4, P. Niles5, and J. Cuadros1, 1Natural History Museum, London, UK 2Planetary Science Institute, Tucson, AZ, USA. 3SUNY Stony Brook, Stony Brook, NY, USA. 4University of New Mexico, Albuquerque, NM, USA. 5NASA Johnson Space Cen- ter, Houston, TX, USA. Introduction: While the surface of Mars may eralogy of deep impact craters was investigated using have had an active hydrosphere early in its history [1], TES, THEMIS, and CRISM data. it is likely that this water retreated to the subsurface Results: We identified ~40 craters of interest in the early on due to loss of the magnetic field and early northern hemisphere, the majority of which occur in atmosphere [2]. This likely resulted in the formation of western Arabia Terra – a potential upwelling zone of two distinct aqueous regimes for Mars from the Late interest [4]. Most of these craters do not contain obvi- Noachian onward: one dominated by redistribution of ous evidence for intra-crater aqueous activity, but surface ice and occasional melting of snow/ice [3], and ~10% contain interior channels and possible lacustrine one dominated by groundwater activity [4]. The exca- features. Most of the craters of interest are blanketed vation of alteration minerals from deep in the crust by by dust, which limits the possibilities for investigating impact craters points to an active, ancient, deep hydro- the mineralogy of intracrater deposits. thermal system [5]. Putative sapping features [6] may One clear exception is McLaughlin Crater (338.6 occur where the groundwater breached the surface. -
Explosive Lava‐Water Interactions in Elysium Planitia, Mars: Geologic and Thermodynamic Constraints on the Formation of the Tartarus Colles Cone Groups Christopher W
JOURNAL OF GEOPHYSICAL RESEARCH, VOL. 115, E09006, doi:10.1029/2009JE003546, 2010 Explosive lava‐water interactions in Elysium Planitia, Mars: Geologic and thermodynamic constraints on the formation of the Tartarus Colles cone groups Christopher W. Hamilton,1 Sarah A. Fagents,1 and Lionel Wilson2 Received 16 November 2009; revised 11 May 2010; accepted 3 June 2010; published 16 September 2010. [1] Volcanic rootless constructs (VRCs) are the products of explosive lava‐water interactions. VRCs are significant because they imply the presence of active lava and an underlying aqueous phase (e.g., groundwater or ice) at the time of their formation. Combined mapping of VRC locations, age‐dating of their host lava surfaces, and thermodynamic modeling of lava‐substrate interactions can therefore constrain where and when water has been present in volcanic regions. This information is valuable for identifying fossil hydrothermal systems and determining relationships between climate, near‐surface water abundance, and the potential development of habitable niches on Mars. We examined the western Tartarus Colles region (25–27°N, 170–171°E) in northeastern Elysium Planitia, Mars, and identified 167 VRC groups with a total area of ∼2000 km2. These VRCs preferentially occur where lava is ∼60 m thick. Crater size‐frequency relationships suggest the VRCs formed during the late to middle Amazonian. Modeling results suggest that at the time of VRC formation, near‐surface substrate was partially desiccated, but that the depth to the midlatitude ice table was ]42 m. This ground ice stability zone is consistent with climate models that predict intermediate obliquity (∼35°) between 75 and 250 Ma, with obliquity excursions descending to ∼25–32°. -
Pre-Mission Insights on the Interior of Mars Suzanne E
Pre-mission InSights on the Interior of Mars Suzanne E. Smrekar, Philippe Lognonné, Tilman Spohn, W. Bruce Banerdt, Doris Breuer, Ulrich Christensen, Véronique Dehant, Mélanie Drilleau, William Folkner, Nobuaki Fuji, et al. To cite this version: Suzanne E. Smrekar, Philippe Lognonné, Tilman Spohn, W. Bruce Banerdt, Doris Breuer, et al.. Pre-mission InSights on the Interior of Mars. Space Science Reviews, Springer Verlag, 2019, 215 (1), pp.1-72. 10.1007/s11214-018-0563-9. hal-01990798 HAL Id: hal-01990798 https://hal.archives-ouvertes.fr/hal-01990798 Submitted on 23 Jan 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. Open Archive Toulouse Archive Ouverte (OATAO ) OATAO is an open access repository that collects the wor of some Toulouse researchers and ma es it freely available over the web where possible. This is an author's version published in: https://oatao.univ-toulouse.fr/21690 Official URL : https://doi.org/10.1007/s11214-018-0563-9 To cite this version : Smrekar, Suzanne E. and Lognonné, Philippe and Spohn, Tilman ,... [et al.]. Pre-mission InSights on the Interior of Mars. (2019) Space Science Reviews, 215 (1). -
Identification of Volcanic Rootless Cones, Ice Mounds, and Impact 3 Craters on Earth and Mars: Using Spatial Distribution As a Remote 4 Sensing Tool
JOURNAL OF GEOPHYSICAL RESEARCH, VOL. 111, XXXXXX, doi:10.1029/2005JE002510, 2006 Click Here for Full Article 2 Identification of volcanic rootless cones, ice mounds, and impact 3 craters on Earth and Mars: Using spatial distribution as a remote 4 sensing tool 1 1 1 2 3 5 B. C. Bruno, S. A. Fagents, C. W. Hamilton, D. M. Burr, and S. M. Baloga 6 Received 16 June 2005; revised 29 March 2006; accepted 10 April 2006; published XX Month 2006. 7 [1] This study aims to quantify the spatial distribution of terrestrial volcanic rootless 8 cones and ice mounds for the purpose of identifying analogous Martian features. Using a 9 nearest neighbor (NN) methodology, we use the statistics R (ratio of the mean NN distance 10 to that expected from a random distribution) and c (a measure of departure from 11 randomness). We interpret R as a measure of clustering and as a diagnostic for 12 discriminating feature types. All terrestrial groups of rootless cones and ice mounds are 13 clustered (R: 0.51–0.94) relative to a random distribution. Applying this same 14 methodology to Martian feature fields of unknown origin similarly yields R of 0.57–0.93, 15 indicating that their spatial distributions are consistent with both ice mound or rootless 16 cone origins, but not impact craters. Each Martian impact crater group has R 1.00 (i.e., 17 the craters are spaced at least as far apart as expected at random). Similar degrees of 18 clustering preclude discrimination between rootless cones and ice mounds based solely on 19 R values. -
NASA Astrobiology Institute 2018 Annual Science Report
A National Aeronautics and Space Administration 2018 Annual Science Report Table of Contents 2018 at the NAI 1 NAI 2018 Teams 2 2018 Team Reports The Evolution of Prebiotic Chemical Complexity and the Organic Inventory 6 of Protoplanetary Disk and Primordial Planets Lead Institution: NASA Ames Research Center Reliving the Past: Experimental Evolution of Major Transitions 18 Lead Institution: Georgia Institute of Technology Origin and Evolution of Organics and Water in Planetary Systems 34 Lead Institution: NASA Goddard Space Flight Center Icy Worlds: Astrobiology at the Water-Rock Interface and Beyond 46 Lead Institution: NASA Jet Propulsion Laboratory Habitability of Hydrocarbon Worlds: Titan and Beyond 60 Lead Institution: NASA Jet Propulsion Laboratory The Origins of Molecules in Diverse Space and Planetary Environments 72 and Their Intramolecular Isotope Signatures Lead Institution: Pennsylvania State University ENIGMA: Evolution of Nanomachines in Geospheres and Microbial Ancestors 80 Lead Institution: Rutgers University Changing Planetary Environments and the Fingerprints of Life 88 Lead Institution: SETI Institute Alternative Earths 100 Lead Institution: University of California, Riverside Rock Powered Life 120 Lead Institution: University of Colorado Boulder NASA Astrobiology Institute iii Annual Report 2018 2018 at the NAI In 2018, the NASA Astrobiology Program announced a plan to transition to a new structure of Research Coordination Networks, RCNs, and simultaneously planned the termination of the NASA Astrobiology Institute -
Astrobiology on Habitable Worlds
Astrobiology on habitable worlds: The case for considering prebiotic chemistry in mission design Aaron Engelhart, Jennifer Blank, Christopher Carr, Zachary Adam, Ariel Anbar, Steven Benner, Donald Burke-Aguero, Aaron Burton, Andrew Ellington, Michael Gaylor, et al. To cite this version: Aaron Engelhart, Jennifer Blank, Christopher Carr, Zachary Adam, Ariel Anbar, et al.. Astrobiology on habitable worlds: The case for considering prebiotic chemistry in mission design. 2020. hal- 03161833 HAL Id: hal-03161833 https://hal.archives-ouvertes.fr/hal-03161833 Submitted on 8 Mar 2021 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. Astrobiology on habitable worlds: The case for considering prebiotic chemistry in mission design Lead author: Aaron E. Engelhart, University of Minnesota. Phone: 612-625-1950 E-mail: [email protected] Co-authors: Jennifer G Blank, NASA Ames Research Center/Blue Marble Space Institute of Science Christopher Carr, Georgia Institute of Technology Henderson James Cleaves, Earth-Life Science Institute Kennda Lynch, Lunar and Planetary Institute/USRA Co-signatories: Zachary Adam, University of Arizona Katarzyna P. Adamala, University of Minnesota Ariel D. Anbar, Arizona State University Laura M. Barge, Jet Propulsion Laboratory David A. Baum, University of Wisconsin-Madison Steven A. -
Conference Program
Conference Program 2018 Conference Chair George K. Tan 2018 Organizing Committee Aaron Pital Jonny Tan Adriana Lozoya Julia McGonigle Becky Rapf Justin Lawrence Ben Intoy Kennda Lynch Bradley Burcar Kimberly Chen Brandon Carroll Marcus Bray Brett McGuire Marshall Seaton Chase Chivers Micha Schaible Chloe Stanton Nadia Szeinbaum Chris Parsons Rio Febrian David Fiahlo Santi Mestre Fos Dedra Eichstedt Scot Sutton Elizabeth Spiers Sheri Motamedi Jay Kroll Zach Duca Jennifer Farrar Proposal Writing Retreat Organizing Committee Becky Rapf (Chair) Julia McGonigle Dedra Eichstedt Zach Duca 2 Sponsors 3 Schedule Monday Tuesday Wednesday Thursday Friday 6/4/18 6/5/18 6/6/18 6/7/18 6/8/18 Breakfast Breakfast Breakfast 8:00AM 8:00-9:00AM 8:00-9:00AM 8:00-9:00AM Talks Talks 9:00AM 1 Warm-up + 3 Talks 1 Warm-up + 3 Talks 9:00AM-10:10AM 9:00AM-10:10AM Coffee Break Coffee Break 10:00AM 10:10AM-10:30AM 10:10AM-10:30AM Talks Talks 4 Talks 4 Talks Field Trip 10:30AM-11:50AM 10:30AM-11:50AM 10:00AM-2:00PM 11:00AM Lunch Lunch 11:50AM-1:00PM 11:50AM-1:00PM 12:00PM Arrival 1:00PM Talks Talks 1 Warm-up + 3 Talks 1 Warm-up + 3 Talks 1:00PM-2:10PM 1:00PM-2:10PM Break 2:00PM Break Break Departure 2:00PM-3:00PM 2:10PM-2:30PM 2:10PM-2:30PM Talks Career Panel Primer 3.0 Info. 3 Talks 2:30PM-3:30PM Session 2:30PM-3:30PM 3:00PM-3:30PM 3:00PM Early Career Town Hall 3:30-4:00PM Posters Posters AGC 2019 Planning 4:00PM 3:30PM-5:30PM 3:30PM-5:30PM 4:00-5:00PM Reception 5:00PM 5:00PM-6:00PM Opening Dinner Dinner On Your Own 6:00PM 5:00PM - 7:00PM 5:30PM - 7:30PM Outreach -
Habitability Models for Astrobiology
Astrobiology, 21, 8. (August, 2021) DOI: 10.1089/ast.2020.2342 Habitability Models for Astrobiology Abel Méndez, Planetary Habitability Laboratory, University of Puerto Rico at Arecibo, Puerto Rico, USA Edgard G. Rivera-Valentín, Lunar and Planetary Institute, USRA, Houston, Texas, USA Dirk Schulze-Makuch, Center for Astronomy and Astrophysics, Technische Universität Berlin, Berlin, Germany; German Research Centre for Geosciences, Section Geomicrobiology, Potsdam, Germany; Leibniz-Institute of Freshwater Ecology and Inland Fisheries, Stechlin, Germany. Justin Filiberto, Lunar and Planetary Institute, USRA, Houston, Texas, USA Ramses M. Ramírez, University of Central Florida, Department of Physics, Orlando, Florida, USA; Space Science Institute, Boulder, Colorado, USA. Tana E. Wood, USDA Forest Service International Institute of Tropical Forestry, San Juan, Puerto Rico, USA Alfonso Dávila, NASA Ames Research Center, Moffett Field, California, USA Chris McKay, NASA Ames Research Center, Moffett Field, California, USA Kevin N. Ortiz Ceballos, Planetary Habitability Laboratory, University of Puerto Rico at Arecibo, Puerto Rico, USA Marcos Jusino-Maldonado, Planetary Habitability Laboratory, University of Puerto Rico at Arecibo, Puerto Rico, USA Nicole J. Torres-Santiago, Planetary Habitability Laboratory, University of Puerto Rico at Arecibo, Puerto Rico, USA Guillermo Nery, Planetary Habitability Laboratory, University of Puerto Rico at Arecibo, Puerto Rico, USA René Heller, Max Planck Institute for Solar System Research; Institute for Astrophysics, -
Martian Groundwaters Though Time and Their Impact on the Mars System
EPSC Abstracts Vol. 13, EPSC-DPS2019-1209-1, 2019 EPSC-DPS Joint Meeting 2019 c Author(s) 2019. CC Attribution 4.0 license. Martian Groundwaters Though Time and Their Impact on the Mars System Bethany L. Ehlmann (1,2) (1) California Institute of Technology, USA, (3) University of Colorado Boulder, USA ([email protected]), (2) Jet Propulsion Laboratory, California Institute of Technology, USA 1. Abstract In situ exploration by Opportunity shows the role of multiple generations of fluids in mineral precipitation Diverse environmental settings with liquid water and dissolution, shaping the sulfate/hematite/chloride are preserved in rocks from ancient Mars [1-4]. An mineralogy of the Burns for-mation sedimentary rocks aspect of this discovery is the prevalence of ancient [17]. Exploration of Noachian materials exposed by terrains with minerals hypothesized to form via impact showed Fe/Mg clay-bearing breccias contain subsurface water-rock reactions, which did not require a warm, wet Mars for extended periods. From orbit, cm-thick leached zones of Al clays from post-impact unambiguous indicator minerals of subsurface waters hydrothermal fluids [18-19]. are hydrothermal/low-grade metamorphic minerals Clearly, Mars hosted multiple types of like prehnite and aqueous mineral assemblages with groundwaters varying in space and time. The drivers compositions isochemical to basalt [5]. Understanding of the chemical diversity are understood in only a few of Martian groundwaters, their chemistry, and their cases. In many cases, sulfur supplied by upwelling importance in the search for life as well as the climate groundwaters leaching basaltic rocks may be system has deepened via continued analyses of orbital sufficient to form sedimentary sulfate deposits without datasets, in situ exploration by Curiosity and invoking atmosphere or magmatic sources [20]. -
Geological and Geochemical Legacy of a Cold Early Mars Eric Gaidos Department of Geology and Geophysics, University of Hawai’I, Honolulu, Hawai’I, USA
JOURNAL OF GEOPHYSICAL RESEARCH, VOL. 108, NO. E6, 5055, doi:10.1029/2002JE002000, 2003 Geological and geochemical legacy of a cold early Mars Eric Gaidos Department of Geology and Geophysics, University of Hawai’i, Honolulu, Hawai’i, USA Giles Marion Desert Research Institute, Reno, Nevada, USA Received 30 October 2002; revised 21 January 2003; accepted 7 February 2003; published 18 June 2003. [1] We consider the hypothesis that Mars never experienced an early warm, wet period and the implications of a continuously cold Martian climate for the hydrology and geochemistry of the planet. Geomorphic evidence previously interpreted to indicate a more temperate early climate can be explained by cold climate processes and the transient flow of liquid water at the surface rather than a terrestrial-like hydrological cycle. In this scenario, freezing and confinement of crustal aquifers lead to the eruption of water or brines to the surface: Hesperian events formed massive ice sheets, and triggered floods that carved the outflow channels, while smaller, present-day aqueous eruptions are responsible for the seepage and gully-like landforms identified in high-resolution imaging. This process may have fluxed a significant volume of groundwater to the surface and the polar caps. A primordial source of groundwater reconciles the present D/H isotopic ratio of the atmosphere with fractionating atmospheric escape and a primordial Martian D/H inferred from hydrous phases of SNC meteorites. A cold early climate and a thin CO2 atmosphere are consistent with the ubiquity of primary igneous minerals and the apparent absence of secondary minerals and copious carbonates on the surface.