1
|
Steele SC, Fu RR, Mittelholz A, Ermakov AI, Citron RI, Lillis RJ. Weak magnetism of Martian impact basins may reflect cooling in a reversing dynamo. Nat Commun 2024; 15:6831. [PMID: 39122701 PMCID: PMC11316139 DOI: 10.1038/s41467-024-51092-4] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 01/15/2024] [Accepted: 07/29/2024] [Indexed: 08/12/2024] Open
Abstract
Understanding the longevity of Mars's dynamo is key to interpreting the planet's atmospheric loss history and the properties of its deep interior. Satellite data showing magnetic lows above many large impact basins formed 4.1-3.7 billion years ago (Ga) have been interpreted as evidence that Mars's dynamo terminated before 4.1 Ga-at least 0.4 Gy before intense late Noachian/early Hesperian hydrological activity. However, evidence for a longer-lived, reversing dynamo from young volcanics and the Martian meteorite ALH 84001 supports an alternative interpretation of Mars's apparently demagnetized basins. To understand how a reversing dynamo would affect basin fields, here we model the cooling and magnetization of 200-2200 km diameter impact basins under a range of Earth-like reversal frequencies. We find that magnetic reversals efficiently reduce field strengths above large basins. In particular, if the magnetic properties of the Martian mantle are similar to most Martian meteorites and late remagnetization of the near surface is widespread, >90% of large ( > 800 km diameter) basins would appear demagnetized at spacecraft altitudes. This ultimately implies that Mars's apparently demagnetized basins do not require an early dynamo cessation. A long-lived and reversing dynamo, unlike alternative scenarios, satisfies all available constraints on Mars's magnetic history.
Collapse
Affiliation(s)
- S C Steele
- Department of Earth and Planetary Sciences, Harvard University, Cambridge, MA, USA.
| | - R R Fu
- Department of Earth and Planetary Sciences, Harvard University, Cambridge, MA, USA
| | - A Mittelholz
- Department of Earth and Planetary Sciences, Harvard University, Cambridge, MA, USA
- Department of Earth Sciences, ETH Zurich, Zurich, Switzerland
| | - A I Ermakov
- Department of Aeronautics and Astronautics, Stanford University, Stanford, CA, USA
| | | | - R J Lillis
- Space Sciences Laboratory, University of California, Berkeley, Berkeley, CA, 94720, USA
| |
Collapse
|
2
|
Clarke JT, Mayyasi M, Bhattacharyya D, Chaufray JY, Schneider N, Jakosky B, Yelle R, Montmessin F, Chaffin M, Curry S, Deighan J, Jain S, Bertaux JL, Cangi E, Crismani M, Evans S, Gupta S, Lefevre F, Holsclaw G, Lo D, McClintock W, Stevens M, Stewart I, Stone S, Mahaffy P, Benna M, Elrod M. Martian atmospheric hydrogen and deuterium: Seasonal changes and paradigm for escape to space. SCIENCE ADVANCES 2024; 10:eadm7499. [PMID: 39058782 PMCID: PMC11277398 DOI: 10.1126/sciadv.adm7499] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Received: 11/03/2023] [Accepted: 06/25/2024] [Indexed: 07/28/2024]
Abstract
Mars' water history is fundamental to understanding Earth-like planet evolution. Water escapes to space as atoms, and hydrogen atoms escape faster than deuterium giving an increase in the residual D/H ratio. The present ratio reflects the total water Mars has lost. Observations with the Mars Atmosphere and Volatile Evolution (MAVEN) and Hubble Space Telescope (HST) spacecraft provide atomic densities and escape rates for H and D. Large increases near perihelion observed each martian year are consistent with a strong upwelling of water vapor. Short-term changes require processes in addition to thermal escape, likely from atmospheric dynamics and superthermal atoms. Including escape from hot atoms, both H and D escape rapidly, and the escape fluxes are limited by resupply from the lower atmosphere. In this paradigm for the escape of water, the D/H ratio of the escaping atoms and the enhancement in water are determined by upwelling water vapor and atmospheric dynamics rather than by the specific details of atomic escape.
Collapse
Affiliation(s)
- John T. Clarke
- Center for Space Physics, Boston University, Boston, MA, USA
| | - Majd Mayyasi
- Center for Space Physics, Boston University, Boston, MA, USA
| | - Dolon Bhattacharyya
- Center for Space Physics, Boston University, Boston, MA, USA
- LASP, University of Colorado, Boulder, CO, USA
| | | | | | | | - Roger Yelle
- Lunar and Planetary Laboratory, University of Arizona, Tucson, AZ, USA
| | | | | | - Shannon Curry
- Space Sciences Laboratory, University of California, Berkeley, CA, USA
| | | | - Sonal Jain
- LASP, University of Colorado, Boulder, CO, USA
| | | | - Erin Cangi
- LASP, University of Colorado, Boulder, CO, USA
| | | | | | | | | | | | - Daniel Lo
- Lunar and Planetary Laboratory, University of Arizona, Tucson, AZ, USA
| | | | - Michael Stevens
- Space Science Division, Naval Research Laboratory, Washington, DC, USA
| | - Ian Stewart
- LASP, University of Colorado, Boulder, CO, USA
| | - Shane Stone
- NASA Goddard Space Flight Center, Greenbelt, MD, USA
| | - Paul Mahaffy
- NASA Goddard Space Flight Center, Greenbelt, MD, USA
| | - Mehdi Benna
- University of Maryland Baltimore County, Baltimore County, MD, USA
| | | |
Collapse
|
3
|
Çelekli A, Zariç ÖE. Breathing life into Mars: Terraforming and the pivotal role of algae in atmospheric genesis. LIFE SCIENCES IN SPACE RESEARCH 2024; 41:181-190. [PMID: 38670646 DOI: 10.1016/j.lssr.2024.03.001] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Key Words] [MESH Headings] [Track Full Text] [Subscribe] [Scholar Register] [Received: 11/20/2023] [Revised: 03/05/2024] [Accepted: 03/08/2024] [Indexed: 04/28/2024]
Abstract
The Martian environment, characterized by extreme aridity, frigid temperatures, and a lack of atmospheric oxygen, presents a formidable challenge for potential terraforming endeavors. This review article synthesizes current research on utilizing algae as biocatalysts in the proposed terraforming of Mars, assessing their capacity to facilitate Martian atmospheric conditions through photosynthetic bioengineering. We analyze the physiological and genetic traits of extremophile algae that equip them for survival in extreme habitats on Earth, which serve as analogs for Martian surface conditions. The potential for these organisms to mediate atmospheric change on Mars is evaluated, specifically their role in biogenic oxygen production and carbon dioxide sequestration. We discuss strategies for enhancing algal strains' resilience and metabolic efficiency, including genetic modification and the development of bioreactors for controlled growth in extraterrestrial environments. The integration of algal systems with existing mechanical and chemical terraforming proposals is also examined, proposing a synergistic approach for establishing a nascent Martian biosphere. Ethical and ecological considerations concerning introducing terrestrial life to extra-planetary bodies are critically appraised. This appraisal includes an examination of potential ecological feedback loops and inherent risks associated with biological terraforming. Biological terraforming is the theoretical process of deliberately altering a planet's atmosphere, temperature, and ecosystem to render it suitable for Earth-like life. The feasibility of a phased introduction of life, starting with microbial taxa and progressing to multicellular organisms, fosters a supportive atmosphere on Mars. By extending the frontier of biotechnological innovation into space, this work contributes to the foundational understanding necessary for one of humanity's most audacious goals-the terraforming of another planet.
Collapse
Affiliation(s)
- Abuzer Çelekli
- Gaziantep University, Faculty of Art and Science, Department of Biology, Gaziantep, Turkey; Gaziantep University, Environmental Research Center (GÜÇAMER), Gaziantep, Turkey.
| | - Özgür Eren Zariç
- Gaziantep University, Faculty of Art and Science, Department of Biology, Gaziantep, Turkey; Gaziantep University, Environmental Research Center (GÜÇAMER), Gaziantep, Turkey
| |
Collapse
|
4
|
Iordachescu A, Eisenstein N, Appleby-Thomas G. Space habitats for bioengineering and surgical repair: addressing the requirement for reconstructive and research tissues during deep-space missions. NPJ Microgravity 2023; 9:23. [PMID: 36966158 PMCID: PMC10039948 DOI: 10.1038/s41526-023-00266-3] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Grants] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 06/30/2022] [Accepted: 03/13/2023] [Indexed: 03/27/2023] Open
Abstract
Numerous technical scenarios have been developed to facilitate a human return to the Moon, and as a testbed for a subsequent mission to Mars. Crews appointed with constructing and establishing planetary bases will require a superior level of physical ability to cope with the operational demands. However, the challenging environments of nearby planets (e.g. geological, atmospheric, gravitational conditions) as well as the lengthy journeys through microgravity, will lead to progressive tissue degradation and an increased susceptibility to injury. The isolation, distance and inability to evacuate in an emergency will require autonomous medical support, as well as a range of facilities and specialised equipment to repair tissue damage on-site. Here, we discuss the design requirements of such a facility, in the form of a habitat that would concomitantly allow tissue substitute production, maintenance and surgical implantation, with an emphasis on connective tissues. The requirements for the individual modules and their operation are identified. Several concepts are assessed, including the presence of adjacent wet lab and medical modules supporting the gradual implementation of regenerative biomaterials and acellular tissue substitutes, leading to eventual tissue grafts and, in subsequent decades, potential tissues/organ-like structures. The latter, currently in early phases of development, are assessed particularly for researching the effects of extreme conditions on representative analogues for astronaut health support. Technical solutions are discussed for bioengineering in an isolated planetary environment with hypogravity, from fluid-gel bath suspended manufacture to cryostorage, cell sourcing and on-site resource utilisation for laboratory infrastructure. Surgical considerations are also discussed.
Collapse
Affiliation(s)
- Alexandra Iordachescu
- School of Chemical Engineering, University of Birmingham, Edgbaston, Birmingham, B15 2TT, United Kingdom.
- Consortium for organotypic research on ageing and microgravity, University of Birmingham, Edgbaston, Birmingham, B15 2TT, United Kingdom.
- Healthcare Technologies Institute, University of Birmingham, Edgbaston, Birmingham, B15 2TT, United Kingdom.
- Cranfield Defence and Security, Cranfield University, Defence Academy of the United Kingdom, Shrivenham, SN6 8LA, United Kingdom.
| | - Neil Eisenstein
- Healthcare Technologies Institute, University of Birmingham, Edgbaston, Birmingham, B15 2TT, United Kingdom
| | - Gareth Appleby-Thomas
- Consortium for organotypic research on ageing and microgravity, University of Birmingham, Edgbaston, Birmingham, B15 2TT, United Kingdom
- Cranfield Defence and Security, Cranfield University, Defence Academy of the United Kingdom, Shrivenham, SN6 8LA, United Kingdom
| |
Collapse
|
5
|
Cox MA, Cavosie AJ, Orr KJ, Daly L, Martin L, Lagain A, Benedix GK, Bland PA. Impact and habitability scenarios for early Mars revisited based on a 4.45-Ga shocked zircon in regolith breccia. SCIENCE ADVANCES 2022; 8:eabl7497. [PMID: 35108046 PMCID: PMC8809541 DOI: 10.1126/sciadv.abl7497] [Citation(s) in RCA: 2] [Impact Index Per Article: 1.0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Download PDF] [Figures] [Subscribe] [Scholar Register] [Received: 09/07/2021] [Accepted: 12/09/2021] [Indexed: 06/14/2023]
Abstract
After formation of a primordial crust, early impacts influenced when habitable conditions may have occurred on Mars. Martian meteorite Northwest Africa (NWA) 7034 is a regolith breccia that contains remnants of the earliest Martian crust. The paucity of shock deformation in NWA 7034 was previously cited as recording a decline in giant impacts by 4.48 billion years and evidence for habitable Mars by 4.2 billion years ago. We present new evidence of high-pressure shock effects in a 4.45-billion year-old zircon from the matrix of NWA 7034. The zircon contains {112} shock twins formed in the central uplift of a complex impact structure after 4.45 billion years and records impact pressures of 20 to 30 gigapascals. The zircon represents the highest shock level reported in NWA 7034 and paired rocks and provides direct physical evidence of large impacts, some potentially life-affecting, that persisted on Mars after 4.48 billion years.
Collapse
Affiliation(s)
- Morgan A. Cox
- Space Science and Technology Centre (SSTC), School of Earth and Planetary Science, Curtin University, Perth, WA 6102, Australia
| | - Aaron J. Cavosie
- Space Science and Technology Centre (SSTC), School of Earth and Planetary Science, Curtin University, Perth, WA 6102, Australia
| | - Kenneth J. Orr
- Space Science and Technology Centre (SSTC), School of Earth and Planetary Science, Curtin University, Perth, WA 6102, Australia
| | - Luke Daly
- School of Geographical and Earth Sciences, University of Glasgow, Glasgow G12 8QQ, UK
| | - Laure Martin
- Centre for Microscopy, Characterisation and Analysis (CMCA), The University of Western Australia, 6 Verdun Street, Perth, WA 6009, Australia
| | - Anthony Lagain
- Space Science and Technology Centre (SSTC), School of Earth and Planetary Science, Curtin University, Perth, WA 6102, Australia
| | - Gretchen K. Benedix
- Space Science and Technology Centre (SSTC), School of Earth and Planetary Science, Curtin University, Perth, WA 6102, Australia
- Department of Earth and Planetary Sciences, Western Australia Museum, Western Australia, Australia
| | - Phil A. Bland
- Space Science and Technology Centre (SSTC), School of Earth and Planetary Science, Curtin University, Perth, WA 6102, Australia
| |
Collapse
|
6
|
Abstract
[Figure: see text].
Collapse
Affiliation(s)
- Erdal Yiğit
- Department of Physics and Astronomy, George Mason University, Fairfax, VA, USA.,Institut für Physik der Atmosphäre, Deutsches Zentrum für Luft- und Raumfahrt, Oberpfaffenhofen, Germany
| |
Collapse
|
7
|
Yang M, Schatz GC. Quasiclassical Trajectory Study of the O( 3P) + CO 2( 1Σ g+) Reaction at Hyperthermal Energies. J Phys Chem A 2021; 125:8626-8634. [PMID: 34585571 DOI: 10.1021/acs.jpca.1c05836] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/28/2022]
Abstract
This paper presents the reaction mechanism, cross sections, and product energy partitioning for the O + CO2 reaction, calculated using Born-Oppenheimer molecular dynamics simulations with the quasiclassical trajectory (BOMD-QCT) method. At collision energies up to 9.5 eV, three reactions, oxygen exchange (above ∼1.5 eV), abstraction (above ∼5.5 eV), and dissociation (above ∼7.5 eV) occur, with abstraction and dissociation involving either an insertion-elimination mechanism or a stripping mechanism. The insertion-elimination mechanism involves the formation of a planar CO3 intermediate which lies 0.52 eV above the ground-state CO2; the energetic barrier for oxygen abstraction via this mechanism is 3.52 eV. Interestingly, the insertion-elimination mechanism predominately contributes to the cross sections at collision energies just above the effective energetic threshold for the abstraction and dissociation reactions; at higher collision energies, the contribution from the stripping mechanism increases and eventually dominates. At a collision energy of 9.5 eV, the cross sections for oxygen exchange, abstraction, and dissociation are 4.17 a02, 1.58 a02, and 0.68 a02, respectively. The lower reaction cross sections, higher effective reaction barrier, and product energy distribution of the stripping mechanism were attributed to the short lifetime (28 fs) of the OCOO species compared with that of the CO3 species (45 fs) that arises in the insertion-elimination mechanism. For the exchange reaction, it is found that roughly 40% of the reactant translational energy ends up in CO2 vibration, which provides a single-collision mechanism to produce highly excited CO2. We also studied intersystem crossing effects using trajectory surface hopping calculations and find no changes compared to single surface (triplet) calculations at energies below 7.5 eV; however, at 7.5 eV and higher the abstraction cross sections are changed by as much as 20%, and the (very small) dissociation cross sections are changed by factors of four or more.
Collapse
Affiliation(s)
- Muwen Yang
- Department of Chemistry and Applied Physics, Northwestern University, 2145 Sheridan Road, Evanston, Illinois 60208-3113, United States
| | - George C Schatz
- Department of Chemistry and Applied Physics, Northwestern University, 2145 Sheridan Road, Evanston, Illinois 60208-3113, United States
| |
Collapse
|
8
|
Abstract
To assess Mars’ potential for both harboring life and providing useable resources for future human exploration, it is of paramount importance to comprehend the water situation on the planet. Therefore, studies have been conducted to determine any evidence of past or present water existence on Mars. While the presence of abundant water on Mars very early in its history is widely accepted, on its modern form, only a fraction of this water can be found, as either ice or locked into the structure of Mars’ plentiful water-rich materials. Water on the planet is evaluated through various evidence such as rocks and minerals, Martian achondrites, low volume transient briny outflows (e.g., dune flows, reactivated gullies, slope streaks, etc.), diurnal shallow soil moisture (e.g., measurements by Curiosity and Phoenix Lander), geomorphic representation (possibly from lakes and river valleys), and groundwater, along with further evidence obtained by probe and rover discoveries. One of the most significant lines of evidence is for an ancient streambed in Gale Crater, implying ancient amounts of “vigorous” water on Mars. Long ago, hospitable conditions for microbial life existed on the surface of Mars, as it was likely periodically wet. However, its current dry surface makes it almost impossible as an appropriate environment for living organisms; therefore, scientists have recognized the planet’s subsurface environments as the best potential locations for exploring life on Mars. As a result, modern research has aimed towards discovering underground water, leading to the discovery of a large amount of underground ice in 2016 by NASA, and a subglacial lake in 2018 by Italian scientists. Nevertheless, the presence of life in Mars’ history is still an open question. In this unifying context, the current review summarizes results from a wide variety of studies and reports related to the history of water on Mars, as well as any related discussions on the possibility of living organism existence on the planet.
Collapse
|
9
|
Habitability of Mars: How Welcoming Are the Surface and Subsurface to Life on the Red Planet? GEOSCIENCES 2019. [DOI: 10.3390/geosciences9090361] [Citation(s) in RCA: 6] [Impact Index Per Article: 1.2] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 11/16/2022]
Abstract
Mars is a planet of great interest in the search for signatures of past or present life beyond Earth. The years of research, and more advanced instrumentation, have yielded a lot of evidence which may be considered by the scientific community as proof of past or present habitability of Mars. Recent discoveries including seasonal methane releases and a subglacial lake are exciting, yet challenging findings. Concurrently, laboratory and environmental studies on the limits of microbial life in extreme environments on Earth broaden our knowledge of the possibility of Mars habitability. In this review, we aim to: (1) Discuss the characteristics of the Martian surface and subsurface that may be conducive to habitability either in the past or at present; (2) discuss laboratory-based studies on Earth that provide us with discoveries on the limits of life; and (3) summarize the current state of knowledge in terms of direction for future research.
Collapse
|
10
|
Yoshida H, Hasegawa H, Katsuta N, Maruyama I, Sirono S, Minami M, Asahara Y, Nishimoto S, Yamaguchi Y, Ichinnorov N, Metcalfe R. Fe-oxide concretions formed by interacting carbonate and acidic waters on Earth and Mars. SCIENCE ADVANCES 2018; 4:eaau0872. [PMID: 30525103 PMCID: PMC6281427 DOI: 10.1126/sciadv.aau0872] [Citation(s) in RCA: 5] [Impact Index Per Article: 0.8] [Reference Citation Analysis] [Abstract] [Grants] [Track Full Text] [Download PDF] [Figures] [Subscribe] [Scholar Register] [Received: 05/05/2018] [Accepted: 10/31/2018] [Indexed: 06/09/2023]
Abstract
Spherical Fe-oxide concretions on Earth, especially in Utah, USA, have been investigated as an analog of hematite spherules found in Meridiani Planum on Mars to support interpretations of water-rock interactions in early Mars. Although several formation mechanisms have been proposed for the Fe-oxide concretions on Earth, it is still unclear whether these mechanisms are viable because a precise formation process and precursor of the concretions are missing. This paper presents evidence that Fe-oxide concretions in Utah and newly found Fe-oxide concretions in Mongolia had spherical calcite concretions as precursors. Different formation stages of calcite and Fe-oxide concretions observed, both in Utah and Mongolia, indicate that calcite concretions initially formed within eolian sandstone strata and were dissolved by infiltrating Fe-rich acidic waters to form spherical FeO(OH) crusts due to pH buffering. The similarity between these Fe-oxide concretions on Earth and the hematite spherule occurrences in Meridiani Planum, combined with evidence of acid sulfate water influences on Mars, suggest that the hematite spherules also formed from dissolution of preexisting carbonate spherules possibly formed under a dense carbon dioxide early martian atmosphere.
Collapse
Affiliation(s)
- H. Yoshida
- Material Research Section, Nagoya University, University Museum, Nagoya, Japan
| | - H. Hasegawa
- Material Research Section, Nagoya University, University Museum, Nagoya, Japan
- Faculty of Science and Technology, Kochi University, Kochi, Japan
| | - N. Katsuta
- Faculty of Education, Gifu University, Gifu, Japan
| | - I. Maruyama
- Graduate School of Environmental Studies, Nagoya University, Nagoya, Japan
| | - S. Sirono
- Graduate School of Environmental Studies, Nagoya University, Nagoya, Japan
| | - M. Minami
- Institute for Space-Earth Environmental Research, Nagoya University, Nagoya, Japan
| | - Y. Asahara
- Graduate School of Environmental Studies, Nagoya University, Nagoya, Japan
| | | | - Y. Yamaguchi
- Graduate School of Environmental Studies, Nagoya University, Nagoya, Japan
| | - N. Ichinnorov
- Institute of Paleontology and Geology, Mongolian Academy of Science, Mongolia
| | - R. Metcalfe
- Quintessa Limited, The Hub, Henley-on-Thames, Oxfordshire, UK
| |
Collapse
|
11
|
Webster CR, Mahaffy PR, Atreya SK, Moores JE, Flesch GJ, Malespin C, McKay CP, Martinez G, Smith CL, Martin-Torres J, Gomez-Elvira J, Zorzano MP, Wong MH, Trainer MG, Steele A, Archer D, Sutter B, Coll PJ, Freissinet C, Meslin PY, Gough RV, House CH, Pavlov A, Eigenbrode JL, Glavin DP, Pearson JC, Keymeulen D, Christensen LE, Schwenzer SP, Navarro-Gonzalez R, Pla-García J, Rafkin SCR, Vicente-Retortillo Á, Kahanpää H, Viudez-Moreiras D, Smith MD, Harri AM, Genzer M, Hassler DM, Lemmon M, Crisp J, Sander SP, Zurek RW, Vasavada AR. Background levels of methane in Mars’ atmosphere show strong seasonal variations. Science 2018; 360:1093-1096. [DOI: 10.1126/science.aaq0131] [Citation(s) in RCA: 189] [Impact Index Per Article: 31.5] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 09/20/2017] [Accepted: 05/04/2018] [Indexed: 11/02/2022]
Abstract
Variable levels of methane in the martian atmosphere have eluded explanation partly because the measurements are not repeatable in time or location. We report in situ measurements at Gale crater made over a 5-year period by the Tunable Laser Spectrometer on the Curiosity rover. The background levels of methane have a mean value 0.41 ± 0.16 parts per billion by volume (ppbv) (95% confidence interval) and exhibit a strong, repeatable seasonal variation (0.24 to 0.65 ppbv). This variation is greater than that predicted from either ultraviolet degradation of impact-delivered organics on the surface or from the annual surface pressure cycle. The large seasonal variation in the background and occurrences of higher temporary spikes (~7 ppbv) are consistent with small localized sources of methane released from martian surface or subsurface reservoirs.
Collapse
|
12
|
High-Resolution Topographic Analyses of Mounds in Southern Acidalia Planitia, Mars: Implications for Possible Mud Volcanism in Submarine and Subaerial Environments. GEOSCIENCES 2018. [DOI: 10.3390/geosciences8050152] [Citation(s) in RCA: 15] [Impact Index Per Article: 2.5] [Reference Citation Analysis] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 11/16/2022]
|
13
|
Bishop JL, Fairén AG, Michalski JR, Gago-Duport L, Baker LL, Velbel MA, Gross C, Rampe EB. Surface clay formation during short-term warmer and wetter conditions on a largely cold ancient Mars. NATURE ASTRONOMY 2018; 2:260-213. [PMID: 32042926 PMCID: PMC7008931 DOI: 10.1038/s41550-017-0377-9] [Citation(s) in RCA: 6] [Impact Index Per Article: 1.0] [Reference Citation Analysis] [Abstract] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Received: 06/19/2017] [Accepted: 12/27/2017] [Indexed: 05/28/2023]
Abstract
The ancient rock record for Mars has long been at odds with climate modelling. The presence of valley networks, dendritic channels and deltas on ancient terrains points towards running water and fluvial erosion on early Mars1, but climate modelling indicates that long-term warm conditions were not sustainable2. Widespread phyllosilicates and other aqueous minerals on the Martian surface3-6 provide additional evidence that an early wet Martian climate resulted in surface weathering. Some of these phyllosilicates formed in subsurface crustal environments5, with no association with the Martian climate, while other phyllosilicate-rich outcrops exhibit layered morphologies and broad stratigraphies7 consistent with surface formation. Here, we develop a new geochemical model for early Mars to explain the formation of these clay-bearing rocks in warm and wet surface locations. We propose that sporadic, short-term warm and wet environments during a generally cold early Mars enabled phyllosilicate formation without requiring long-term warm and wet conditions. We conclude that Mg-rich clay-bearing rocks with lateral variations in mixed Fe/Mg smectite, chlorite, talc, serpentine and zeolite occurrences formed in subsurface hydrothermal environments, whereas dioctahedral (Al/Fe3+-rich) smectite and widespread vertical horizonation of Fe/Mg smectites, clay assemblages and sulphates formed in variable aqueous environments on the surface of Mars. Our model for aluminosilicate formation on Mars is consistent with the observed geological features, diversity of aqueous mineralogies in ancient surface rocks and state-of-the-art palaeoclimate scenarios.
Collapse
Affiliation(s)
- Janice L. Bishop
- SETI Institute, Mountain View, CA, USA
- National Aeronautics and Space Administration’s Ames Research Center, Moffett Field, CA, USA
| | - Alberto G. Fairén
- Centro de Astrobiología (Consejo Superior de Investigaciones Científicas-Instituto Nacional de Técnica Aeroespacial), Madrid, Spain
- Cornell University, Ithaca, NY, USA
| | - Joseph R. Michalski
- Department of Earth Sciences & Laboratory for Space Research, University of Hong Kong, Hong Kong, China
| | | | | | - Michael A. Velbel
- Michigan State University, East Lansing, MI, USA
- Smithsonian Institution, Washington, DC, USA
| | | | - Elizabeth B. Rampe
- National Aeronautics and Space Administration-Johnson Space Center, Houston, TX, USA
| |
Collapse
|
14
|
|
15
|
Cabrol NA. The Coevolution of Life and Environment on Mars: An Ecosystem Perspective on the Robotic Exploration of Biosignatures. ASTROBIOLOGY 2018; 18:1-27. [PMID: 29252008 PMCID: PMC5779243 DOI: 10.1089/ast.2017.1756] [Citation(s) in RCA: 6] [Impact Index Per Article: 1.0] [Reference Citation Analysis] [Abstract] [MESH Headings] [Track Full Text] [Subscribe] [Scholar Register] [Received: 08/29/2017] [Accepted: 11/27/2017] [Indexed: 05/09/2023]
Abstract
Earth's biological and environmental evolution are intertwined and inseparable. This coevolution has become a fundamental concept in astrobiology and is key to the search for life beyond our planet. In the case of Mars, whether a coevolution took place is unknown, but analyzing the factors at play shows the uniqueness of each planetary experiment regardless of similarities. Early Earth and early Mars shared traits. However, biological processes on Mars, if any, would have had to proceed within the distinctive context of an irreversible atmospheric collapse, greater climate variability, and specific planetary characteristics. In that, Mars is an important test bed for comparing the effects of a unique set of spatiotemporal changes on an Earth-like, yet different, planet. Many questions remain unanswered about Mars' early environment. Nevertheless, existing data sets provide a foundation for an intellectual framework where notional coevolution models can be explored. In this framework, the focus is shifted from planetary-scale habitability to the prospect of habitats, microbial ecotones, pathways to biological dispersal, biomass repositories, and their meaning for exploration. Critically, as we search for biosignatures, this focus demonstrates the importance of starting to think of early Mars as a biosphere and vigorously integrating an ecosystem approach to landing site selection and exploration. Key Words: Astrobiology-Biosignatures-Coevolution of Earth and life-Mars. Astrobiology 18, 1-27.
Collapse
|
16
|
Beblo-Vranesevic K, Bohmeier M, Perras AK, Schwendner P, Rabbow E, Moissl-Eichinger C, Cockell CS, Pukall R, Vannier P, Marteinsson VT, Monaghan EP, Ehrenfreund P, Garcia-Descalzo L, Gómez F, Malki M, Amils R, Gaboyer F, Westall F, Cabezas P, Walter N, Rettberg P. The responses of an anaerobic microorganism, Yersinia intermedia MASE-LG-1 to individual and combined simulated Martian stresses. PLoS One 2017; 12:e0185178. [PMID: 29069099 PMCID: PMC5656303 DOI: 10.1371/journal.pone.0185178] [Citation(s) in RCA: 10] [Impact Index Per Article: 1.4] [Reference Citation Analysis] [Abstract] [MESH Headings] [Grants] [Track Full Text] [Download PDF] [Figures] [Journal Information] [Subscribe] [Scholar Register] [Received: 03/03/2017] [Accepted: 09/07/2017] [Indexed: 11/18/2022] Open
Abstract
The limits of life of aerobic microorganisms are well understood, but the responses of anaerobic microorganisms to individual and combined extreme stressors are less well known. Motivated by an interest in understanding the survivability of anaerobic microorganisms under Martian conditions, we investigated the responses of a new isolate, Yersinia intermedia MASE-LG-1 to individual and combined stresses associated with the Martian surface. This organism belongs to an adaptable and persistent genus of anaerobic microorganisms found in many environments worldwide. The effects of desiccation, low pressure, ionizing radiation, varying temperature, osmotic pressure, and oxidizing chemical compounds were investigated. The strain showed a high tolerance to desiccation, with a decline of survivability by four orders of magnitude during a storage time of 85 days. Exposure to X-rays resulted in dose-dependent inactivation for exposure up to 600 Gy while applied doses above 750 Gy led to complete inactivation. The effects of the combination of desiccation and irradiation were additive and the survivability was influenced by the order in which they were imposed. Ionizing irradiation and subsequent desiccation was more deleterious than vice versa. By contrast, the presence of perchlorates was not found to significantly affect the survival of the Yersinia strain after ionizing radiation. These data show that the organism has the capacity to survive and grow in physical and chemical stresses, imposed individually or in combination that are associated with Martian environment. Eventually it lost its viability showing that many of the most adaptable anaerobic organisms on Earth would be killed on Mars today.
Collapse
Affiliation(s)
- Kristina Beblo-Vranesevic
- Radiation Biology Department, Institute of Aerospace Medicine, German Aerospace Center (DLR), Cologne, Germany
- * E-mail:
| | - Maria Bohmeier
- Radiation Biology Department, Institute of Aerospace Medicine, German Aerospace Center (DLR), Cologne, Germany
| | - Alexandra K. Perras
- Department of Internal Medicine, Medical University of Graz, Graz, Austria
- Department of Microbiology and Archaea, University of Regensburg, Regensburg, Germany
| | - Petra Schwendner
- School of Physics and Astronomy, UK Center for Astrobiology, University of Edinburgh, Edinburgh, United Kingdom
| | - Elke Rabbow
- Radiation Biology Department, Institute of Aerospace Medicine, German Aerospace Center (DLR), Cologne, Germany
| | - Christine Moissl-Eichinger
- Department of Internal Medicine, Medical University of Graz, Graz, Austria
- BioTechMed Graz, Graz, Austria
| | - Charles S. Cockell
- School of Physics and Astronomy, UK Center for Astrobiology, University of Edinburgh, Edinburgh, United Kingdom
| | - Rüdiger Pukall
- German Collection of Microorganisms and Cell Cultures, Leibniz Institute DSMZ, Braunschweig, Germany
| | | | - Viggo T. Marteinsson
- MATIS—Prokaria, Reykjavík, Iceland
- Faculty of Food Science and Nutrition, University of Iceland, Reykjavík, Iceland
| | | | - Pascale Ehrenfreund
- Leiden Observatory, Universiteit Leiden, Leiden, Netherland
- Space Policy Institute, George Washington University, Washington DC, United States of America
| | - Laura Garcia-Descalzo
- Instituto Nacional de Técnica Aeroespacial—Centro de Astrobiología (INTA-CAB), Madrid, Spain
| | - Felipe Gómez
- Instituto Nacional de Técnica Aeroespacial—Centro de Astrobiología (INTA-CAB), Madrid, Spain
| | | | | | - Frédéric Gaboyer
- Centre de Biophysique Moléculaire, Centre National de la Recherche Scientifique (CNRS), Orléans, France
| | - Frances Westall
- Centre de Biophysique Moléculaire, Centre National de la Recherche Scientifique (CNRS), Orléans, France
| | | | | | - Petra Rettberg
- Radiation Biology Department, Institute of Aerospace Medicine, German Aerospace Center (DLR), Cologne, Germany
| |
Collapse
|
17
|
Cockell CS, Bush T, Bryce C, Direito S, Fox-Powell M, Harrison JP, Lammer H, Landenmark H, Martin-Torres J, Nicholson N, Noack L, O'Malley-James J, Payler SJ, Rushby A, Samuels T, Schwendner P, Wadsworth J, Zorzano MP. Habitability: A Review. ASTROBIOLOGY 2016; 16:89-117. [PMID: 26741054 DOI: 10.1089/ast.2015.1295] [Citation(s) in RCA: 94] [Impact Index Per Article: 11.8] [Reference Citation Analysis] [Abstract] [MESH Headings] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 05/25/2023]
Abstract
Habitability is a widely used word in the geoscience, planetary science, and astrobiology literature, but what does it mean? In this review on habitability, we define it as the ability of an environment to support the activity of at least one known organism. We adopt a binary definition of "habitability" and a "habitable environment." An environment either can or cannot sustain a given organism. However, environments such as entire planets might be capable of supporting more or less species diversity or biomass compared with that of Earth. A clarity in understanding habitability can be obtained by defining instantaneous habitability as the conditions at any given time in a given environment required to sustain the activity of at least one known organism, and continuous planetary habitability as the capacity of a planetary body to sustain habitable conditions on some areas of its surface or within its interior over geological timescales. We also distinguish between surface liquid water worlds (such as Earth) that can sustain liquid water on their surfaces and interior liquid water worlds, such as icy moons and terrestrial-type rocky planets with liquid water only in their interiors. This distinction is important since, while the former can potentially sustain habitable conditions for oxygenic photosynthesis that leads to the rise of atmospheric oxygen and potentially complex multicellularity and intelligence over geological timescales, the latter are unlikely to. Habitable environments do not need to contain life. Although the decoupling of habitability and the presence of life may be rare on Earth, it may be important for understanding the habitability of other planetary bodies.
Collapse
Affiliation(s)
- C S Cockell
- 1 UK Centre for Astrobiology, School of Physics and Astronomy, University of Edinburgh , Edinburgh, UK
| | - T Bush
- 1 UK Centre for Astrobiology, School of Physics and Astronomy, University of Edinburgh , Edinburgh, UK
| | - C Bryce
- 1 UK Centre for Astrobiology, School of Physics and Astronomy, University of Edinburgh , Edinburgh, UK
| | - S Direito
- 1 UK Centre for Astrobiology, School of Physics and Astronomy, University of Edinburgh , Edinburgh, UK
| | - M Fox-Powell
- 1 UK Centre for Astrobiology, School of Physics and Astronomy, University of Edinburgh , Edinburgh, UK
| | - J P Harrison
- 1 UK Centre for Astrobiology, School of Physics and Astronomy, University of Edinburgh , Edinburgh, UK
| | - H Lammer
- 2 Austrian Academy of Sciences, Space Research Institute , Graz, Austria
| | - H Landenmark
- 1 UK Centre for Astrobiology, School of Physics and Astronomy, University of Edinburgh , Edinburgh, UK
| | - J Martin-Torres
- 3 Division of Space Technology, Department of Computer Science, Electrical and Space Engineering, Luleå University of Technology , Kiruna, Sweden; and Instituto Andaluz de Ciencias de la Tierra (CSIC-UGR), Armilla, Granada, Spain
| | - N Nicholson
- 1 UK Centre for Astrobiology, School of Physics and Astronomy, University of Edinburgh , Edinburgh, UK
| | - L Noack
- 4 Department of Reference Systems and Planetology, Royal Observatory of Belgium , Brussels, Belgium
| | - J O'Malley-James
- 5 School of Physics and Astronomy, University of St Andrews , St Andrews, UK; now at the Carl Sagan Institute, Cornell University, Ithaca, NY, USA
| | - S J Payler
- 1 UK Centre for Astrobiology, School of Physics and Astronomy, University of Edinburgh , Edinburgh, UK
| | - A Rushby
- 6 Centre for Ocean and Atmospheric Science (COAS), School of Environmental Sciences, University of East Anglia , Norwich, UK
| | - T Samuels
- 1 UK Centre for Astrobiology, School of Physics and Astronomy, University of Edinburgh , Edinburgh, UK
| | - P Schwendner
- 1 UK Centre for Astrobiology, School of Physics and Astronomy, University of Edinburgh , Edinburgh, UK
| | - J Wadsworth
- 1 UK Centre for Astrobiology, School of Physics and Astronomy, University of Edinburgh , Edinburgh, UK
| | - M P Zorzano
- 3 Division of Space Technology, Department of Computer Science, Electrical and Space Engineering, Luleå University of Technology , Kiruna, Sweden; and Instituto Andaluz de Ciencias de la Tierra (CSIC-UGR), Armilla, Granada, Spain
- 7 Centro de Astrobiología (CSIC-INTA) , Torrejón de Ardoz, Madrid, Spain
| |
Collapse
|
18
|
Hu R, Kass DM, Ehlmann BL, Yung YL. Tracing the fate of carbon and the atmospheric evolution of Mars. Nat Commun 2015; 6:10003. [PMID: 26600077 PMCID: PMC4673500 DOI: 10.1038/ncomms10003] [Citation(s) in RCA: 23] [Impact Index Per Article: 2.6] [Reference Citation Analysis] [Abstract] [Track Full Text] [Download PDF] [Figures] [Journal Information] [Subscribe] [Scholar Register] [Received: 07/17/2015] [Accepted: 10/26/2015] [Indexed: 11/18/2022] Open
Abstract
The climate of Mars likely evolved from a warmer, wetter early state to the cold, arid current state. However, no solutions for this evolution have previously been found to satisfy the observed geological features and isotopic measurements of the atmosphere. Here we show that a family of solutions exist, invoking no missing reservoirs or loss processes. Escape of carbon via CO photodissociation and sputtering enriches heavy carbon (13C) in the Martian atmosphere, partially compensated by moderate carbonate precipitation. The current atmospheric 13C/12C and rock and soil carbonate measurements indicate an early atmosphere with a surface pressure <1 bar. Only scenarios with large amounts of carbonate formation in open lakes permit higher values up to 1.8 bar. The evolutionary scenarios are fully testable with data from the MAVEN mission and further studies of the isotopic composition of carbonate in the Martian rock record through time. Mars likely evolved from a warmer, wetter early state to the cold, arid current climate, but this evolution is not reflected in recent observations and measurements. Here, the authors derive quantitative constraints on the atmospheric pressure through time, identifying a mechanism that explains the carbon data.
Collapse
Affiliation(s)
- Renyu Hu
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, California 91109, USA.,Division of Geological and Planetary Sciences, California Institute of Technology, Pasadena, California 91125, USA
| | - David M Kass
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, California 91109, USA
| | - Bethany L Ehlmann
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, California 91109, USA.,Division of Geological and Planetary Sciences, California Institute of Technology, Pasadena, California 91125, USA
| | - Yuk L Yung
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, California 91109, USA.,Division of Geological and Planetary Sciences, California Institute of Technology, Pasadena, California 91125, USA
| |
Collapse
|
19
|
Earth-like aqueous debris-flow activity on Mars at high orbital obliquity in the last million years. Nat Commun 2015; 6:7543. [PMID: 26102485 PMCID: PMC4557294 DOI: 10.1038/ncomms8543] [Citation(s) in RCA: 37] [Impact Index Per Article: 4.1] [Reference Citation Analysis] [Abstract] [Track Full Text] [Download PDF] [Figures] [Journal Information] [Subscribe] [Scholar Register] [Received: 10/25/2014] [Accepted: 05/19/2015] [Indexed: 12/03/2022] Open
Abstract
Liquid water is currently extremely rare on Mars, but was more abundant during periods of high obliquity in the last few millions of years. This is testified by the widespread occurrence of mid-latitude gullies: small catchment-fan systems. However, there are no direct estimates of the amount and frequency of liquid water generation during these periods. Here we determine debris-flow size, frequency and associated water volumes in Istok crater, and show that debris flows occurred at Earth-like frequencies during high-obliquity periods in the last million years on Mars. Results further imply that local accumulations of snow/ice within gullies were much more voluminous than currently predicted; melting must have yielded centimetres of liquid water in catchments; and recent aqueous activity in some mid-latitude craters was much more frequent than previously anticipated. It is thought that water flowed on the surface of Mars in the geological past during periods of high orbital obliquity. Here, the authors assess how much liquid water was present and suggest that debris flows occurred at Earth-like frequencies during high-obliquity periods in the past million years.
Collapse
|
20
|
Evidence for indigenous nitrogen in sedimentary and aeolian deposits from the Curiosity rover investigations at Gale crater, Mars. Proc Natl Acad Sci U S A 2015; 112:4245-50. [PMID: 25831544 DOI: 10.1073/pnas.1420932112] [Citation(s) in RCA: 145] [Impact Index Per Article: 16.1] [Reference Citation Analysis] [Abstract] [Key Words] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/18/2022] Open
Abstract
The Sample Analysis at Mars (SAM) investigation on the Mars Science Laboratory (MSL) Curiosity rover has detected oxidized nitrogen-bearing compounds during pyrolysis of scooped aeolian sediments and drilled sedimentary deposits within Gale crater. Total N concentrations ranged from 20 to 250 nmol N per sample. After subtraction of known N sources in SAM, our results support the equivalent of 110-300 ppm of nitrate in the Rocknest (RN) aeolian samples, and 70-260 and 330-1,100 ppm nitrate in John Klein (JK) and Cumberland (CB) mudstone deposits, respectively. Discovery of indigenous martian nitrogen in Mars surface materials has important implications for habitability and, specifically, for the potential evolution of a nitrogen cycle at some point in martian history. The detection of nitrate in both wind-drifted fines (RN) and in mudstone (JK, CB) is likely a result of N2 fixation to nitrate generated by thermal shock from impact or volcanic plume lightning on ancient Mars. Fixed nitrogen could have facilitated the development of a primitive nitrogen cycle on the surface of ancient Mars, potentially providing a biochemically accessible source of nitrogen.
Collapse
|
21
|
Tomkinson T, Lee MR, Mark DF, Smith CL. Sequestration of Martian CO2 by mineral carbonation. Nat Commun 2014; 4:2662. [PMID: 24149494 PMCID: PMC4354006 DOI: 10.1038/ncomms3662] [Citation(s) in RCA: 17] [Impact Index Per Article: 1.7] [Reference Citation Analysis] [Abstract] [Track Full Text] [Download PDF] [Figures] [Journal Information] [Subscribe] [Scholar Register] [Received: 06/11/2013] [Accepted: 09/24/2013] [Indexed: 12/03/2022] Open
Abstract
Carbonation is the water-mediated replacement of silicate minerals, such as olivine, by carbonate, and is commonplace in the Earth’s crust. This reaction can remove significant quantities of CO2 from the atmosphere and store it over geological timescales. Here we present the first direct evidence for CO2 sequestration and storage on Mars by mineral carbonation. Electron beam imaging and analysis show that olivine and a plagioclase feldspar-rich mesostasis in the Lafayette meteorite have been replaced by carbonate. The susceptibility of olivine to replacement was enhanced by the presence of smectite veins along which CO2-rich fluids gained access to grain interiors. Lafayette was partially carbonated during the Amazonian, when liquid water was available intermittently and atmospheric CO2 concentrations were close to their present-day values. Earlier in Mars’ history, when the planet had a much thicker atmosphere and an active hydrosphere, carbonation is likely to have been an effective mechanism for sequestration of CO2. The mechanism by which Mars lost its early dense and carbon dioxide-rich atmosphere remains relatively unknown. Here, via mineralogical analysis of the Lafayette Martian meteorite, Tomkinson et al. infer that carbonation was an effective carbon dioxide sequestration mechanism on an early, water-rich Mars.
Collapse
Affiliation(s)
- Tim Tomkinson
- Scottish Universities Environmental Research Centre, Rankine Avenue, Scottish Enterprise Technology Park, East Kilbride G75 0QF, UK
| | | | | | | |
Collapse
|
22
|
Groemer G, Sattler B, Weisleitner K, Hunger L, Kohstall C, Frisch A, Józefowicz M, Meszyński S, Storrie-Lombardi M, Bothe C, Boyd A, Dinkelaker A, Dissertori M, Fasching D, Fischer M, Föger D, Foresta L, Frischauf N, Fritsch L, Fuchs H, Gautsch C, Gerard S, Goetzloff L, Gołebiowska I, Gorur P, Groemer G, Groll P, Haider C, Haider O, Hauth E, Hauth S, Hettrich S, Jais W, Jones N, Taj-Eddine K, Karl A, Kauerhoff T, Khan MS, Kjeldsen A, Klauck J, Losiak A, Luger M, Luger T, Luger U, McArthur J, Moser L, Neuner J, Orgel C, Ori GG, Paternesi R, Peschier J, Pfeil I, Prock S, Radinger J, Ragonig C, Ramirez B, Ramo W, Rampey M, Sams A, Sams E, Sams S, Sandu O, Sans A, Sansone P, Scheer D, Schildhammer D, Scornet Q, Sejkora N, Soucek A, Stadler A, Stummer F, Stumptner W, Taraba M, Tlustos R, Toferer E, Turetschek T, Winter E, Zanella-Kux K. Field trial of a dual-wavelength fluorescent emission (L.I.F.E.) instrument and the Magma White rover during the MARS2013 Mars analog mission. ASTROBIOLOGY 2014; 14:391-405. [PMID: 24823800 DOI: 10.1089/ast.2013.1081] [Citation(s) in RCA: 2] [Impact Index Per Article: 0.2] [Reference Citation Analysis] [Abstract] [MESH Headings] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 06/03/2023]
Abstract
Abstract We have developed a portable dual-wavelength laser fluorescence spectrometer as part of a multi-instrument optical probe to characterize mineral, organic, and microbial species in extreme environments. Operating at 405 and 532 nm, the instrument was originally designed for use by human explorers to produce a laser-induced fluorescence emission (L.I.F.E.) spectral database of the mineral and organic molecules found in the microbial communities of Earth's cryosphere. Recently, our team had the opportunity to explore the strengths and limitations of the instrument when it was deployed on a remote-controlled Mars analog rover. In February 2013, the instrument was deployed on board the Magma White rover platform during the MARS2013 Mars analog field mission in the Kess Kess formation near Erfoud, Morocco. During these tests, we followed tele-science work flows pertinent to Mars surface missions in a simulated spaceflight environment. We report on the L.I.F.E. instrument setup, data processing, and performance during field trials. A pilot postmission laboratory analysis determined that rock samples acquired during the field mission exhibited a fluorescence signal from the Sun-exposed side characteristic of chlorophyll a following excitation at 405 nm. A weak fluorescence response to excitation at 532 nm may have originated from another microbial photosynthetic pigment, phycoerythrin, but final assignment awaits development of a comprehensive database of mineral and organic fluorescence spectra. No chlorophyll fluorescence signal was detected from the shaded underside of the samples.
Collapse
Affiliation(s)
- Gernot Groemer
- 1 Institute of Ecology, University of Innsbruck , Innsbruck, Austria
| | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | |
Collapse
|
23
|
Wong MH, Atreya SK, Mahaffy PN, Franz HB, Malespin C, Trainer MG, Stern JC, Conrad PG, Manning HLK, Pepin RO, Becker RH, McKay CP, Owen TC, Navarro-González R, Jones JH, Jakosky BM, Steele A. Isotopes of nitrogen on Mars: Atmospheric measurements by Curiosity's mass spectrometer. GEOPHYSICAL RESEARCH LETTERS 2013; 40:6033-6037. [PMID: 26074632 PMCID: PMC4459194 DOI: 10.1002/2013gl057840] [Citation(s) in RCA: 14] [Impact Index Per Article: 1.3] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 09/03/2013] [Revised: 11/18/2013] [Accepted: 11/09/2013] [Indexed: 05/23/2023]
Abstract
[1] The Sample Analysis at Mars (SAM) instrument suite on the Mars Science Laboratory (MSL) measured a Mars atmospheric14N/15N ratio of 173 ± 11 on sol 341 of the mission, agreeing with Viking's measurement of 168 ± 17. The MSL/SAM value was based on Quadrupole Mass Spectrometer measurements of an enriched atmospheric sample, with CO2 and H2O removed. Doubly ionized nitrogen data at m/z 14 and 14.5 had the highest signal/background ratio, with results confirmed by m/z 28 and 29 data. Gases in SNC meteorite glasses have been interpreted as mixtures containing a Martian atmospheric component, based partly on distinctive14N/15N and40Ar/14N ratios. Recent MSL/SAM measurements of the40Ar/14N ratio (0.51 ± 0.01) are incompatible with the Viking ratio (0.35 ± 0.08). The meteorite mixing line is more consistent with the atmospheric composition measured by Viking than by MSL.
Collapse
Affiliation(s)
- Michael H Wong
- Department of Atmospheric, Oceanic, and Space Sciences, University of MichiganAnn Arbor, Michigan, USA
- Astronomy Department, University of CaliforniaBerkeley, California, USA
| | - Sushil K Atreya
- Department of Atmospheric, Oceanic, and Space Sciences, University of MichiganAnn Arbor, Michigan, USA
| | - Paul N Mahaffy
- Code 699, NASA Goddard Space Flight CenterGreenbelt, Maryland, USA
| | - Heather B Franz
- Code 699, NASA Goddard Space Flight CenterGreenbelt, Maryland, USA
| | - Charles Malespin
- Code 699, NASA Goddard Space Flight CenterGreenbelt, Maryland, USA
| | | | - Jennifer C Stern
- Code 699, NASA Goddard Space Flight CenterGreenbelt, Maryland, USA
| | - Pamela G Conrad
- Code 699, NASA Goddard Space Flight CenterGreenbelt, Maryland, USA
| | | | - Robert O Pepin
- School of Physics and Astronomy, University of MinnesotaMinneapolis, Minnesota, USA
| | - Richard H Becker
- School of Physics and Astronomy, University of MinnesotaMinneapolis, Minnesota, USA
| | | | - Tobias C Owen
- Institute for Astronomy, University of Hawai‘i at MānoaHonolulu, Hawaii, USA
| | | | | | | | - Andrew Steele
- Geophysical Laboratory, Carnegie Institution of WashingtonWashington, District of Columbia, USA
| |
Collapse
|
24
|
Hassler DM, Zeitlin C, Wimmer-Schweingruber RF, Ehresmann B, Rafkin S, Eigenbrode JL, Brinza DE, Weigle G, Böttcher S, Böhm E, Burmeister S, Guo J, Köhler J, Martin C, Reitz G, Cucinotta FA, Kim MH, Grinspoon D, Bullock MA, Posner A, Gómez-Elvira J, Vasavada A, Grotzinger JP. Mars' surface radiation environment measured with the Mars Science Laboratory's Curiosity rover. Science 2013; 343:1244797. [PMID: 24324275 DOI: 10.1126/science.1244797] [Citation(s) in RCA: 226] [Impact Index Per Article: 20.5] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/02/2022]
Abstract
The Radiation Assessment Detector (RAD) on the Mars Science Laboratory's Curiosity rover began making detailed measurements of the cosmic ray and energetic particle radiation environment on the surface of Mars on 7 August 2012. We report and discuss measurements of the absorbed dose and dose equivalent from galactic cosmic rays and solar energetic particles on the martian surface for ~300 days of observations during the current solar maximum. These measurements provide insight into the radiation hazards associated with a human mission to the surface of Mars and provide an anchor point with which to model the subsurface radiation environment, with implications for microbial survival times of any possible extant or past life, as well as for the preservation of potential organic biosignatures of the ancient martian environment.
Collapse
|
25
|
Humayun M, Nemchin A, Zanda B, Hewins RH, Grange M, Kennedy A, Lorand JP, Göpel C, Fieni C, Pont S, Deldicque D. Origin and age of the earliest Martian crust from meteorite NWA 7533. Nature 2013; 503:513-6. [PMID: 24256724 DOI: 10.1038/nature12764] [Citation(s) in RCA: 240] [Impact Index Per Article: 21.8] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 07/04/2013] [Accepted: 10/10/2013] [Indexed: 11/09/2022]
Abstract
The ancient cratered terrain of the southern highlands of Mars is thought to hold clues to the planet's early differentiation, but until now no meteoritic regolith breccias have been recovered from Mars. Here we show that the meteorite Northwest Africa (NWA) 7533 (paired with meteorite NWA 7034) is a polymict breccia consisting of a fine-grained interclast matrix containing clasts of igneous-textured rocks and fine-grained clast-laden impact melt rocks. High abundances of meteoritic siderophiles (for example nickel and iridium) found throughout the rock reach a level in the fine-grained portions equivalent to 5 per cent CI chondritic input, which is comparable to the highest levels found in lunar breccias. Furthermore, analyses of three leucocratic monzonite clasts show a correlation between nickel, iridium and magnesium consistent with differentiation from impact melts. Compositionally, all the fine-grained material is alkalic basalt, chemically identical (except for sulphur, chlorine and zinc) to soils from Gusev crater. Thus, we propose that NWA 7533 is a Martian regolith breccia. It contains zircons for which we measured an age of 4,428 ± 25 million years, which were later disturbed 1,712 ± 85 million years ago. This evidence for early crustal differentiation implies that the Martian crust, and its volatile inventory, formed in about the first 100 million years of Martian history, coeval with earliest crust formation on the Moon and the Earth. In addition, incompatible element abundances in clast-laden impact melt rocks and interclast matrix provide a geochemical estimate of the average thickness of the Martian crust (50 kilometres) comparable to that estimated geophysically.
Collapse
Affiliation(s)
- M Humayun
- Department of Earth, Ocean and Atmospheric Science, and National High Magnetic Field Laboratory, Florida State University, Tallahassee, Florida 32310, USA
| | | | | | | | | | | | | | | | | | | | | |
Collapse
|
26
|
Westall F, Loizeau D, Foucher F, Bost N, Betrand M, Vago J, Kminek G. Habitability on Mars from a microbial point of view. ASTROBIOLOGY 2013; 13:887-97. [PMID: 24015806 DOI: 10.1089/ast.2013.1000] [Citation(s) in RCA: 33] [Impact Index Per Article: 3.0] [Reference Citation Analysis] [Abstract] [MESH Headings] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 05/20/2023]
Abstract
Extraterrestrial habitability is a complex notion. We briefly review what is known about the origin of life on Earth, that is, life based on carbon chemistry and water. We then discuss habitable conditions (past and present) for established life and for the survival of microorganisms. Based on these elements, we propose to use the term habitable only for conditions necessary for the origin of life, the proliferation of life, and the survival of life. Not covered by this term would be conditions necessary for prebiotic chemistry and conditions that would allow the recognition of extinct or hibernating life. Finally, we apply this concept to the potential emergence of life on Mars where suitable conditions for life to start, proliferate, and survive have been heterogeneous throughout its history. These considerations have a profound impact on the nature and distribution of eventual traces of martian life, or any precursor, and must therefore inform our search-for-life strategies.
Collapse
Affiliation(s)
- Frances Westall
- 1 CNRS-OSUC-Centre de Biophysique Moléculaire , Orléans, France
| | | | | | | | | | | | | |
Collapse
|
27
|
Webster CR, Mahaffy PR, Flesch GJ, Niles PB, Jones JH, Leshin LA, Atreya SK, Stern JC, Christensen LE, Owen T, Franz H, Pepin RO, Steele A. Isotope Ratios of H, C, and O in CO
2
and H
2
O of the Martian Atmosphere. Science 2013; 341:260-3. [PMID: 23869013 DOI: 10.1126/science.1237961] [Citation(s) in RCA: 46] [Impact Index Per Article: 4.2] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/02/2022]
Affiliation(s)
- Chris R. Webster
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109, USA
| | | | - Gregory J. Flesch
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109, USA
| | | | | | | | | | | | - Lance E. Christensen
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109, USA
| | - Tobias Owen
- University of Hawaii, Honolulu, HI 96822, USA
| | - Heather Franz
- NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA
| | | | - Andrew Steele
- Carnegie Institution of Washington, Washington, DC 20015, USA
| | | |
Collapse
|
28
|
Abbey W, Salas E, Bhartia R, Beegle LW. The Mojave vadose zone: a subsurface biosphere analogue for Mars. ASTROBIOLOGY 2013; 13:637-646. [PMID: 23848498 DOI: 10.1089/ast.2012.0948] [Citation(s) in RCA: 1] [Impact Index Per Article: 0.1] [Reference Citation Analysis] [Abstract] [MESH Headings] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 06/02/2023]
Abstract
If life ever evolved on the surface of Mars, it is unlikely that it would still survive there today, but as Mars evolved from a wet planet to an arid one, the subsurface environment may have presented a refuge from increasingly hostile surface conditions. Since the last glacial maximum, the Mojave Desert has experienced a similar shift from a wet to a dry environment, giving us the opportunity to study here on Earth how subsurface ecosystems in an arid environment adapt to increasingly barren surface conditions. In this paper, we advocate studying the vadose zone ecosystem of the Mojave Desert as an analogue for possible subsurface biospheres on Mars. We also describe several examples of Mars-like terrain found in the Mojave region and discuss ecological insights that might be gained by a thorough examination of the vadose zone in these specific terrains. Examples described include distributary fans (deltas, alluvial fans, etc.), paleosols overlain by basaltic lava flows, and evaporite deposits.
Collapse
Affiliation(s)
- William Abbey
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109, USA
| | | | | | | |
Collapse
|
29
|
Milbury C, Schubert G, Raymond CA, Smrekar SE, Langlais B. The history of Mars' dynamo as revealed by modeling magnetic anomalies near Tyrrhenus Mons and Syrtis Major. ACTA ACUST UNITED AC 2012. [DOI: 10.1029/2012je004099] [Citation(s) in RCA: 27] [Impact Index Per Article: 2.3] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/10/2022]
|
30
|
Kereszturi A. Review of wet environment types on Mars with focus on duration and volumetric issues. ASTROBIOLOGY 2012; 12:586-600. [PMID: 22794300 DOI: 10.1089/ast.2011.0686] [Citation(s) in RCA: 4] [Impact Index Per Article: 0.3] [Reference Citation Analysis] [Abstract] [MESH Headings] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 06/01/2023]
Abstract
The astrobiological significance of certain environment types on Mars strongly depends on the temperature, duration, and chemistry of liquid water that was present there in the past. Recent works have focused on the identification of signs of ancient water on Mars, as it is more difficult to estimate the above-mentioned parameters. In this paper, two important factors are reviewed, the duration and the volume of water at different environment types on past and present Mars. Using currently available information, we can only roughly estimate these values, but as environment types show characteristic differences in this respect, it is worth comparing them and the result may have importance for research in astrobiology. Impact-induced and geothermal hydrothermal systems, lakes, and valley networks were in existence on Mars over the course of from 10(2) to 10(6) years, although they would have experienced substantially different temperature regimes. Ancient oceans, as well as water in outflow channels and gullies, and at the microscopic scale as interfacial water layers, would have had inherently different times of duration and overall volume: oceans may have endured from 10(4) to 10(6) years, while interfacial water would have had the smallest volume and residence time of liquid phase on Mars. Martian wet environments with longer residence times of liquid water are believed to have existed for that amount of time necessary for life to develop on Earth between the Late Heavy Bombardment and the age of the earliest fossil record. The results of this review show the necessity for more detailed analysis of conditions within geothermal heat-induced systems to reconstruct the conditions during weathering and mineral alteration, as well as to search for signs of reoccurring wet periods in ancient crater lakes.
Collapse
Affiliation(s)
- Akos Kereszturi
- Konkoly Thege Miklos Astronomical Institute, Research Centre for Astronomy and Earth Sciences, Hungarian Academy of Sciences, Budapest, Hungary.
| |
Collapse
|
31
|
Ehresmann B, Burmeister S, Wimmer-Schweingruber RF, Reitz G. Influence of higher atmospheric pressure on the Martian radiation environment: Implications for possible habitability in the Noachian epoch. ACTA ACUST UNITED AC 2011. [DOI: 10.1029/2011ja016616] [Citation(s) in RCA: 16] [Impact Index Per Article: 1.2] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
Affiliation(s)
- B. Ehresmann
- Institute for Experimental and Applied Physics; Christian Albrechts University Kiel; Kiel Germany
| | - S. Burmeister
- Institute for Experimental and Applied Physics; Christian Albrechts University Kiel; Kiel Germany
| | | | - G. Reitz
- Institute of Aerospace Medicine, Radiation Biology; German Aerospace Center; Cologne Germany
| |
Collapse
|
32
|
Cousins CR, Crawford IA. Volcano-ice interaction as a microbial habitat on Earth and Mars. ASTROBIOLOGY 2011; 11:695-710. [PMID: 21877914 DOI: 10.1089/ast.2010.0550] [Citation(s) in RCA: 5] [Impact Index Per Article: 0.4] [Reference Citation Analysis] [Abstract] [MESH Headings] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 05/31/2023]
Abstract
Volcano-ice interaction has been a widespread geological process on Earth that continues to occur to the present day. The interaction between volcanic activity and ice can generate substantial quantities of liquid water, together with steep thermal and geochemical gradients typical of hydrothermal systems. Environments available for microbial colonization within glaciovolcanic systems are wide-ranging and include the basaltic lava edifice, subglacial caldera meltwater lakes, glacier caves, and subsurface hydrothermal systems. There is widespread evidence of putative volcano-ice interaction on Mars throughout its history and at a range of latitudes. Therefore, it is possible that life on Mars may have exploited these habitats, much in the same way as has been observed on Earth. The sedimentary and mineralogical deposits resulting from volcano-ice interaction have the potential to preserve evidence of any indigenous microbial populations. These include jökulhlaup (subglacial outflow) sedimentary deposits, hydrothermal mineral deposits, basaltic lava flows, and subglacial lacustrine deposits. Here, we briefly review the evidence for volcano-ice interactions on Mars and discuss the geomicrobiology of volcano-ice habitats on Earth. In addition, we explore the potential for the detection of these environments on Mars and any biosignatures these deposits may contain.
Collapse
Affiliation(s)
- Claire R Cousins
- Department of Earth and Planetary Sciences, Birkbeck College, University of London, London, UK.
| | | |
Collapse
|
33
|
Phillips RJ, Davis BJ, Tanaka KL, Byrne S, Mellon MT, Putzig NE, Haberle RM, Kahre MA, Campbell BA, Carter LM, Smith IB, Holt JW, Smrekar SE, Nunes DC, Plaut JJ, Egan AF, Titus TN, Seu R. Massive CO
2
Ice Deposits Sequestered in the South Polar Layered Deposits of Mars. Science 2011; 332:838-41. [DOI: 10.1126/science.1203091] [Citation(s) in RCA: 190] [Impact Index Per Article: 14.6] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/02/2022]
Affiliation(s)
- Roger J. Phillips
- Planetary Science Directorate, Southwest Research Institute, Boulder, CO 80302, USA and Department of Earth and Planetary Sciences, Washington University, St. Louis, MO 63130, USA
| | - Brian J. Davis
- Department of Space Studies, Southwest Research Institute, Boulder, CO 80302, USA
| | - Kenneth L. Tanaka
- Astrogeology Science Center, U.S. Geological Survey, Flagstaff, AZ 86001, USA
| | - Shane Byrne
- Lunar and Planetary Laboratory, University of Arizona, Tucson, AZ 85721, USA
| | - Michael T. Mellon
- Laboratory for Atmospheric and Space Physics, University of Colorado, Boulder, CO 80303, USA
| | - Nathaniel E. Putzig
- Department of Space Studies, Southwest Research Institute, Boulder, CO 80302, USA
| | - Robert M. Haberle
- Space Science and Astrobiology Division, National Aeronautics and Space Administration (NASA) Ames Research Center, Moffett Field, CA 94035, USA
| | - Melinda A. Kahre
- Bay Area Environmental Research Institute/NASA Ames Research Center, Moffett Field, CA 94035, USA
| | - Bruce A. Campbell
- Center for Earth and Planetary Studies, Smithsonian Institution, Washington, DC 20013, USA
| | - Lynn M. Carter
- Science and Exploration Directorate, NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA
| | - Isaac B. Smith
- Institute for Geophysics, Jackson School of Geosciences, University of Texas, Austin, TX 78758, USA
| | - John W. Holt
- Institute for Geophysics, Jackson School of Geosciences, University of Texas, Austin, TX 78758, USA
| | - Suzanne E. Smrekar
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109, USA
| | - Daniel C. Nunes
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109, USA
| | - Jeffrey J. Plaut
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109, USA
| | - Anthony F. Egan
- Department of Space Operations, Southwest Research Institute, Boulder, CO 80302, USA
| | - Timothy N. Titus
- Astrogeology Science Center, U.S. Geological Survey, Flagstaff, AZ 86001, USA
| | - Roberto Seu
- Department of Information Engineering, Electronics and Telecommunications, Sapienza University of Rome, 18-00184 Rome, Italy
| |
Collapse
|
34
|
|
35
|
Hynek BM, Beach M, Hoke MRT. Updated global map of Martian valley networks and implications for climate and hydrologic processes. ACTA ACUST UNITED AC 2010. [DOI: 10.1029/2009je003548] [Citation(s) in RCA: 312] [Impact Index Per Article: 22.3] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
|
36
|
Resistance of Microorganisms to Extreme Environmental Conditions and Its Contribution to Astrobiology. SUSTAINABILITY 2010. [DOI: 10.3390/su2061602] [Citation(s) in RCA: 55] [Impact Index Per Article: 3.9] [Reference Citation Analysis] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 11/16/2022]
|
37
|
The Mars Astrobiology Explorer-Cacher (MAX-C): a potential rover mission for 2018. Final report of the Mars Mid-Range Rover Science Analysis Group (MRR-SAG) October 14, 2009. ASTROBIOLOGY 2010; 10:127-163. [PMID: 20298148 DOI: 10.1089/ast.2010.0462] [Citation(s) in RCA: 1] [Impact Index Per Article: 0.1] [Reference Citation Analysis] [Abstract] [MESH Headings] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 05/29/2023]
Abstract
This report documents the work of the Mid-Range Rover Science Analysis Group (MRR-SAG), which was assigned to formulate a concept for a potential rover mission that could be launched to Mars in 2018. Based on programmatic and engineering considerations as of April 2009, our deliberations assumed that the potential mission would use the Mars Science Laboratory (MSL) sky-crane landing system and include a single solar-powered rover. The mission would also have a targeting accuracy of approximately 7 km (semimajor axis landing ellipse), a mobility range of at least 10 km, and a lifetime on the martian surface of at least 1 Earth year. An additional key consideration, given recently declining budgets and cost growth issues with MSL, is that the proposed rover must have lower cost and cost risk than those of MSL--this is an essential consideration for the Mars Exploration Program Analysis Group (MEPAG). The MRR-SAG was asked to formulate a mission concept that would address two general objectives: (1) conduct high priority in situ science and (2) make concrete steps toward the potential return of samples to Earth. The proposed means of achieving these two goals while balancing the trade-offs between them are described here in detail. We propose the name Mars Astrobiology Explorer-Cacher(MAX-C) to reflect the dual purpose of this potential 2018 rover mission.
Collapse
|
38
|
Abstract
Accretion left the terrestrial planets depleted in volatile components. Here I examine evidence for the hypothesis that the Moon and the Earth were essentially dry immediately after the formation of the Moon-by a giant impact on the proto-Earth-and only much later gained volatiles through accretion of wet material delivered from beyond the asteroid belt. This view is supported by U-Pb and I-Xe chronologies, which show that water delivery peaked approximately 100 million years after the isolation of the Solar System. Introduction of water into the terrestrial mantle triggered plate tectonics, which may have been crucial for the emergence of life. This mechanism may also have worked for the young Venus, but seems to have failed for Mars.
Collapse
|
39
|
Hoke MRT, Hynek BM. Roaming zones of precipitation on ancient Mars as recorded in valley networks. ACTA ACUST UNITED AC 2009. [DOI: 10.1029/2008je003247] [Citation(s) in RCA: 61] [Impact Index Per Article: 4.1] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
Affiliation(s)
- Monica R. T. Hoke
- Department of Astrophysical and Planetary ScienceUniversity of Colorado at Boulder Boulder Colorado USA
- Laboratory for Atmospheric and Space PhysicsUniversity of Colorado at Boulder Boulder Colorado USA
| | - Brian M. Hynek
- Laboratory for Atmospheric and Space PhysicsUniversity of Colorado at Boulder Boulder Colorado USA
- Department of Geological SciencesUniversity of Colorado at Boulder Boulder Colorado USA
| |
Collapse
|
40
|
Poulet F, Beaty DW, Bibring JP, Bish D, Bishop JL, Noe Dobrea E, Mustard JF, Petit S, Roach LH. Key scientific questions and key investigations from the first international conference on Martian phyllosilicates. ASTROBIOLOGY 2009; 9:257-267. [PMID: 19400732 DOI: 10.1089/ast.2009.0335] [Citation(s) in RCA: 2] [Impact Index Per Article: 0.1] [Reference Citation Analysis] [Abstract] [MESH Headings] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 05/27/2023]
Abstract
Minerals and their occurrences can tell us about the chemistry, pressure, and temperatures of past environments on Mars and thus allow inferences about the potential for habitability. Thanks to recent space exploration, a new vision is emerging wherein Mars hosted environmental conditions of potential astrobiological relevance. This epoch is identified by the presence of phyllosilicate-bearing deposits, which are generally contained in very ancient basement rocks. In October 2008, over 100 planetary scientists representing 11 countries met in Paris to assess and discuss the relevance of martian phyllosilicates. The conference was structured to promote the discussion and debate of key scientific questions and key essential investigations. The purpose of this report is to document the current state of knowledge related to martian phyllosilicates and to ascertain which questions remain to be addressed: What are the basic characteristics of the phyllosilicate minerals on Mars? What are the genetic mechanisms by which phyllosilicate minerals have formed on Mars? What is the relationship between the phyllosilicate minerals observed in martian meteorites and those detected from orbit? What are the implications of phyllosilicate-bearing rocks for the development of prebiotic chemistry and the preservation of biosignatures? The most promising investigations to address these questions are presented.
Collapse
Affiliation(s)
- François Poulet
- Institut d'Astrophysique Spatiale, CNRS/Université Paris-Sud, Orsay, France.
| | | | | | | | | | | | | | | | | |
Collapse
|
41
|
Usui T, McSween HY, Clark BC. Petrogenesis of high-phosphorous Wishstone Class rocks in Gusev Crater, Mars. ACTA ACUST UNITED AC 2008. [DOI: 10.1029/2008je003225] [Citation(s) in RCA: 31] [Impact Index Per Article: 1.9] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
|
42
|
Jellinek AM, Johnson CL, Schubert G. Constraints on the elastic thickness, heat flow, and melt production at early Tharsis from topography and magnetic field observations. ACTA ACUST UNITED AC 2008. [DOI: 10.1029/2007je003005] [Citation(s) in RCA: 16] [Impact Index Per Article: 1.0] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/10/2022]
|
43
|
Cleaves HJ, Chalmers JH, Lazcano A, Miller SL, Bada JL. A reassessment of prebiotic organic synthesis in neutral planetary atmospheres. ORIGINS LIFE EVOL B 2008; 38:105-15. [PMID: 18204914 DOI: 10.1007/s11084-007-9120-3] [Citation(s) in RCA: 130] [Impact Index Per Article: 8.1] [Reference Citation Analysis] [Abstract] [MESH Headings] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 09/17/2007] [Accepted: 12/09/2007] [Indexed: 11/25/2022]
Abstract
The action of an electric discharge on reduced gas mixtures such as H(2)O, CH(4) and NH(3) (or N(2)) results in the production of several biologically important organic compounds including amino acids. However, it is now generally held that the early Earth's atmosphere was likely not reducing, but was dominated by N(2) and CO(2). The synthesis of organic compounds by the action of electric discharges on neutral gas mixtures has been shown to be much less efficient. We show here that contrary to previous reports, significant amounts of amino acids are produced from neutral gas mixtures. The low yields previously reported appear to be the outcome of oxidation of the organic compounds during hydrolytic workup by nitrite and nitrate produced in the reactions. The yield of amino acids is greatly increased when oxidation inhibitors, such as ferrous iron, are added prior to hydrolysis. Organic synthesis from neutral atmospheres may have depended on the oceanic availability of oxidation inhibitors as well as on the nature of the primitive atmosphere itself. The results reported here suggest that endogenous synthesis from neutral atmospheres may be more important than previously thought.
Collapse
Affiliation(s)
- H James Cleaves
- Geophysical Laboratory, Carnegie Institution of Washington, Washington, DC, 20015, USA
| | | | | | | | | |
Collapse
|
44
|
Chaufray JY, Modolo R, Leblanc F, Chanteur G, Johnson RE, Luhmann JG. Mars solar wind interaction: Formation of the Martian corona and atmospheric loss to space. ACTA ACUST UNITED AC 2007. [DOI: 10.1029/2007je002915] [Citation(s) in RCA: 101] [Impact Index Per Article: 5.9] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
|
45
|
O'Neill C, Lenardic A, Jellinek AM, Kiefer WS. Melt propagation and volcanism in mantle convection simulations, with applications for Martian volcanic and atmospheric evolution. ACTA ACUST UNITED AC 2007. [DOI: 10.1029/2006je002799] [Citation(s) in RCA: 38] [Impact Index Per Article: 2.2] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/10/2022]
|
46
|
Chevrier V, Poulet F, Bibring JP. Early geochemical environment of Mars as determined from thermodynamics of phyllosilicates. Nature 2007; 448:60-3. [PMID: 17611538 DOI: 10.1038/nature05961] [Citation(s) in RCA: 153] [Impact Index Per Article: 9.0] [Reference Citation Analysis] [Abstract] [MESH Headings] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 09/29/2006] [Accepted: 05/22/2007] [Indexed: 11/09/2022]
Abstract
Images of geomorphological features that seem to have been produced by the action of liquid water have been considered evidence for wet surface conditions on early Mars. Moreover, the recent identification of large deposits of phyllosilicates, associated with the ancient Noachian terrains suggests long-timescale weathering of the primary basaltic crust by liquid water. It has been proposed that a greenhouse effect resulting from a carbon-dioxide-rich atmosphere sustained the temperate climate required to maintain liquid water on the martian surface during the Noachian. The apparent absence of carbonates and the low escape rates of carbon dioxide, however, are indicative of an early martian atmosphere with low levels of carbon dioxide. Here we investigate the geochemical conditions prevailing on the surface of Mars during the Noachian period using calculations of the aqueous equilibria of phyllosilicates. Our results show that Fe3+-rich phyllosilicates probably precipitated under weakly acidic to alkaline pH, an environment different from that of the following period, which was dominated by strongly acid weathering that led to the sulphate deposits identified on Mars. Thermodynamic calculations demonstrate that the oxidation state of the martian surface was already high, supporting early escape of hydrogen. Finally, equilibrium with carbonates implies that phyllosilicate precipitation occurs preferentially at a very low partial pressure of carbon dioxide. We suggest that the possible absence of Noachian carbonates more probably resulted from low levels of atmospheric carbon dioxide, rather than primary acidic conditions. Other greenhouse gases may therefore have played a part in sustaining a warm and wet climate on the early Mars.
Collapse
Affiliation(s)
- Vincent Chevrier
- W. M. Keck Laboratory for Space Simulation, Arkansas Center for Space and Planetary Sciences, MUSE 202, University of Arkansas, Fayetteville, Arkansas 72701, USA.
| | | | | |
Collapse
|
47
|
Summers DP, Khare B. Nitrogen fixation on early Mars and other terrestrial planets: experimental demonstration of abiotic fixation reactions to nitrite and nitrate. ASTROBIOLOGY 2007; 7:333-41. [PMID: 17480164 DOI: 10.1089/ast.2006.0032] [Citation(s) in RCA: 18] [Impact Index Per Article: 1.1] [Reference Citation Analysis] [Abstract] [MESH Headings] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 05/15/2023]
Abstract
Understanding the abiotic fixation of nitrogen is critical to understanding planetary evolution and the potential origin of life on terrestrial planets. Nitrogen, an essential biochemical element, is certainly necessary for life as we know it to arise. The loss of atmospheric nitrogen can result in an incapacity to sustain liquid water and impact planetary habitability and hydrological processes that shape the surface. However, our current understanding of how such fixation may occur is almost entirely theoretical. This work experimentally examines the chemistry, in both gas and aqueous phases, that would occur from the formation of NO and CO by the shock heating of a model carbon dioxide/nitrogen atmosphere such as is currently thought to exist on early terrestrial planets. The results show that two pathways exist for the abiotic fixation of nitrogen from the atmosphere into the crust: one via HNO and another via NO(2). Fixation via HNO, which requires liquid water, could represent fixation on a planet with liquid water (and hence would also be a source of nitrogen for the origin of life). The pathway via NO(2) does not require liquid water and shows that fixation could occur even when liquid water has been lost from a planet's surface (for example, continuing to remove nitrogen through NO(2) reaction with ice, adsorbed water, etc.).
Collapse
Affiliation(s)
- David P Summers
- SETI Institute, c/o NASA Ames Research Center, Moffett Field, California 94035-1000, USA.
| | | |
Collapse
|
48
|
|
49
|
Bibring JP, Langevin Y, Mustard JF, Poulet F, Arvidson R, Gendrin A, Gondet B, Mangold N, Pinet P, Forget F, Berthé M, Bibring JP, Gendrin A, Gomez C, Gondet B, Jouglet D, Poulet F, Soufflot A, Vincendon M, Combes M, Drossart P, Encrenaz T, Fouchet T, Merchiorri R, Belluci G, Altieri F, Formisano V, Capaccioni F, Cerroni P, Coradini A, Fonti S, Korablev O, Kottsov V, Ignatiev N, Moroz V, Titov D, Zasova L, Loiseau D, Mangold N, Pinet P, Douté S, Schmitt B, Sotin C, Hauber E, Hoffmann H, Jaumann R, Keller U, Arvidson R, Mustard JF, Duxbury T, Forget F, Neukum G. Global Mineralogical and Aqueous Mars History Derived from OMEGA/Mars Express Data. Science 2006; 312:400-4. [PMID: 16627738 DOI: 10.1126/science.1122659] [Citation(s) in RCA: 270] [Impact Index Per Article: 15.0] [Reference Citation Analysis] [Abstract] [MESH Headings] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/02/2022]
Abstract
Global mineralogical mapping of Mars by the Observatoire pour la Mineralogie, l'Eau, les Glaces et l'Activité (OMEGA) instrument on the European Space Agency's Mars Express spacecraft provides new information on Mars' geological and climatic history. Phyllosilicates formed by aqueous alteration very early in the planet's history (the "phyllocian" era) are found in the oldest terrains; sulfates were formed in a second era (the "theiikian" era) in an acidic environment. Beginning about 3.5 billion years ago, the last era (the "siderikian") is dominated by the formation of anhydrous ferric oxides in a slow superficial weathering, without liquid water playing a major role across the planet.
Collapse
Affiliation(s)
- Jean-Pierre Bibring
- Institut d'Astrophysique Spatiale (IAS), Bâtiment 121, 91405 Orsay Campus, France
| | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | |
Collapse
|
50
|
Hurowitz JA, McLennan SM, Tosca NJ, Arvidson RE, Michalski JR, Ming DW, Schröder C, Squyres SW. In situ and experimental evidence for acidic weathering of rocks and soils on Mars. ACTA ACUST UNITED AC 2006. [DOI: 10.1029/2005je002515] [Citation(s) in RCA: 135] [Impact Index Per Article: 7.5] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
Affiliation(s)
- J. A. Hurowitz
- Department of Geosciences; State University of New York at Stony Brook; Stony Brook New York USA
| | - S. M. McLennan
- Department of Geosciences; State University of New York at Stony Brook; Stony Brook New York USA
| | - N. J. Tosca
- Department of Geosciences; State University of New York at Stony Brook; Stony Brook New York USA
| | - R. E. Arvidson
- Department of Earth and Planetary Sciences; Washington University; St. Louis Missouri USA
| | - J. R. Michalski
- Department of Geological Sciences; Arizona State University; Tempe Arizona USA
| | - D. W. Ming
- NASA Johnson Space Center; Houston Texas USA
| | - C. Schröder
- Institut für Anorganische und Analytische Chemie; Johannes Gutenberg-Universität; Mainz Germany
| | - S. W. Squyres
- Department of Astronomy; Cornell University; Ithaca New York USA
| |
Collapse
|