3D Modeling of Supersaturated H2O/H2O2 on Early Mars Climate During the Noachia

Total Page:16

File Type:pdf, Size:1020Kb

3D Modeling of Supersaturated H2O/H2O2 on Early Mars Climate During the Noachia EPSC Abstracts Vol. 15, EPSC2021-302, 2021, updated on 30 Sep 2021 https://doi.org/10.5194/epsc2021-302 Europlanet Science Congress 2021 © Author(s) 2021. This work is distributed under the Creative Commons Attribution 4.0 License. 3D Modeling of Supersaturated H2O/H2O2 on Early Mars Climate during the Noachia Antony Delavois1, François Forget1, Martin Turbet2, and Ehouarn Millour1 1Laboratoire Météorologie Dynamique, Institut Pierre Simon Laplace, Paris, France 2Observatoire Astronomique de l’Université de Genève, Chemin Pegasi 51, 1290 Sauverny,Switzerland The climate of Mars during its first billion years is one of the most intriguing question in our understanding of the Solar System. The planet was host of a large amount of liquid water flowing on the surface throughout the Noachian era, approximatively 4Gya. Geomorphological observations is the main evidence for liquid water since valley networks and lakes are still visible on the surface, although dry nowadays. Different studies have tried to reproduce the conditions that may have occured on the planet, trying to find an atmospheric process or composition that could solve the Faint Young Sun Paradox. Theses modeling studies, through the use of 3-dimensional Global Climate Models struggled to warm sufficiently the past climate of Mars, even considering different greenhouse gases, the role of clouds, meteoritic impact or even volcanism (XXX). However, the presence of H2 could be an interesting solution for a sustainable warming as some recent studies suggest (Turbet and Forget, 2021). Another recent study (Ito et al. 2020) suggested that H2O2 might be a convincing candidate but has to be in high supersaturation ratio in the atmosphere, even though it only used a simplified 1D model and relatively high supersaturation levels. We try here to explore more in detail the scenario of supersaturated H2O2 and H2O, that also might be a specy able to provide a sufficient global warming under supersaturated conditions or through the formation of high altitude clouds. Since H2O is the major source of H2O2 in the atmosphere, it is important to assess whether the H2O content in the atmosphere is enough to provide high quantities of H2O2. We also try to constrain the theoritical supersaturation level of H2O/H2O2 that will allow the warming of the climate above 273K, but with a detailled 3D GCM simulation. Even if we do not tackle the question whether the supersaturation hypothesis is realistic or not, these results give a better understanding of what would be Early Mars' climate under such conditions. Powered by TCPDF (www.tcpdf.org).
Recommended publications
  • Mars, the Nearest Habitable World – a Comprehensive Program for Future Mars Exploration
    Mars, the Nearest Habitable World – A Comprehensive Program for Future Mars Exploration Report by the NASA Mars Architecture Strategy Working Group (MASWG) November 2020 Front Cover: Artist Concepts Top (Artist concepts, left to right): Early Mars1; Molecules in Space2; Astronaut and Rover on Mars1; Exo-Planet System1. Bottom: Pillinger Point, Endeavour Crater, as imaged by the Opportunity rover1. Credits: 1NASA; 2Discovery Magazine Citation: Mars Architecture Strategy Working Group (MASWG), Jakosky, B. M., et al. (2020). Mars, the Nearest Habitable World—A Comprehensive Program for Future Mars Exploration. MASWG Members • Bruce Jakosky, University of Colorado (chair) • Richard Zurek, Mars Program Office, JPL (co-chair) • Shane Byrne, University of Arizona • Wendy Calvin, University of Nevada, Reno • Shannon Curry, University of California, Berkeley • Bethany Ehlmann, California Institute of Technology • Jennifer Eigenbrode, NASA/Goddard Space Flight Center • Tori Hoehler, NASA/Ames Research Center • Briony Horgan, Purdue University • Scott Hubbard, Stanford University • Tom McCollom, University of Colorado • John Mustard, Brown University • Nathaniel Putzig, Planetary Science Institute • Michelle Rucker, NASA/JSC • Michael Wolff, Space Science Institute • Robin Wordsworth, Harvard University Ex Officio • Michael Meyer, NASA Headquarters ii Mars, the Nearest Habitable World October 2020 MASWG Table of Contents Mars, the Nearest Habitable World – A Comprehensive Program for Future Mars Exploration Table of Contents EXECUTIVE SUMMARY ..........................................................................................................................
    [Show full text]
  • Mid-Latitude Ice on Mars: a Science Target for Planetary Climate Histories and an Exploration Target for in Situ Resources
    Mid-Latitude Ice on Mars: A Science Target for Planetary Climate Histories and an Exploration Target for In Situ Resources A White Paper submitted to the Planetary Sciences Decadal Survey 2023–2032 Primary Contact: Ali M. Bramson, Purdue University ([email protected]) Authors: Ali M. Bramson1,2 John (Jack) W. Holt2 Eric I. Petersen2,12 Chimira Andres3 Suniti Karunatillake8 Nathaniel E. Putzig6 Jonathan Bapst4 Aditya Khuller9 Hanna G. Sizemore6 Patricio Becerra5 Michael T. Mellon10 Isaac B. Smith6,13 Samuel W. Courville6 Gareth A. Morgan6 David E. Stillman14 Colin M. Dundas7 Rachel W. Obbard11 Paul Wooster15 Shannon M. Hibbard3 Matthew R. Perry6 1Purdue University, 2University of Arizona, 3University of Western Ontario CA, 4Jet Propulsion Laboratory, California Institute of Technology, 5University of Bern CH, 6Planetary Science Institute, 7U.S. Geological Survey, 8Louisiana State University, 9Arizona State University, 10Cornell University, 11SETI Institute, 12University of Alaska Fairbanks, 13York University, 14Southwest Research Institute, 15SpaceX Signatories: Ken Herkenhoff, U.S. Geological Survey Alfred McEwen, U. of Arizona David M. Hollibaugh Baker, NASA GSFC Wendy Calvin, U. of Nevada Reno Stefano Nerozzi, U. of Arizona Nicolas Thomas, U. of Bern, CH Serina Diniega, NASA JPL Paul Hayne, U. of Colorado Boulder Jeffrey Plaut, NASA JPL/Caltech Kim Seelos, JHU/APL Charity Phillips-Lander, SwRI Shane Byrne, U. of Arizona Cynthia Dinwiddie, SwRI Devanshu Jha, MVJ College of Eng., IN Aymeric Spiga, LMD/Sorbonne Université, FR Michael S. Veto, Ball Aerospace Andreas Johnsson, U. of Gothenburg, SE Matthew Chojnacki, PSI Michael Mischna, NASA JPL/Caltech Jacob Widmer, Representing Self Adrian J. Brown, Plancius Research, LLC Carol Stoker, NASA Ames Noora Alsaeed, CU Boulder, LASP Alberto G.
    [Show full text]
  • Seasonal and Interannual Variability of Solar Radiation at Spirit, Opportunity and Curiosity Landing Sites
    Seasonal and interannual variability of solar radiation at Spirit, Opportunity and Curiosity landing sites Álvaro VICENTE-RETORTILLO1, Mark T. LEMMON2, Germán M. MARTÍNEZ3, Francisco VALERO4, Luis VÁZQUEZ5, Mª Luisa MARTÍN6 1Departamento de Física de la Tierra, Astronomía y Astrofísica II, Universidad Complutense de Madrid, Madrid, Spain, [email protected]. 2Department of Atmospheric Sciences, Texas A&M University, College Station, TX, USA, [email protected]. 3Department of Climate and Space Sciences and Engineering, University of Michigan, Ann Arbor, MI, USA, [email protected]. 4Departamento de Física de la Tierra, Astronomía y Astrofísica II, Universidad Complutense de Madrid, Madrid, Spain, [email protected]. 5Departamento de Matemática Aplicada, Universidad Complutense de Madrid, Madrid, Spain, [email protected]. 6Departamento de Matemática Aplicada, Universidad de Valladolid, Segovia, Spain, [email protected]. Received: 14/04/2016 Accepted: 22/09/2016 Abstract In this article we characterize the radiative environment at the landing sites of NASA's Mars Exploration Rover (MER) and Mars Science Laboratory (MSL) missions. We use opacity values obtained at the surface from direct imaging of the Sun and our radiative transfer model COMIMART to analyze the seasonal and interannual variability of the daily irradiation at the MER and MSL landing sites. In addition, we analyze the behavior of the direct and diffuse components of the solar radiation at these landing sites. Key words: Solar radiation; Mars Exploration Rovers; Mars Science Laboratory; opacity, dust; radiative transfer model; Mars exploration. Variabilidad estacional e interanual de la radiación solar en las coordenadas de aterrizaje de Spirit, Opportunity y Curiosity Resumen El presente artículo está dedicado a la caracterización del entorno radiativo en los lugares de aterrizaje de las misiones de la NASA de Mars Exploration Rover (MER) y de Mars Science Laboratory (MSL).
    [Show full text]
  • FROM WET PLANET to RED PLANET Current and Future Exploration Is Shaping Our Understanding of How the Climate of Mars Changed
    FROM WET PLANET TO RED PLANET Current and future exploration is shaping our understanding of how the climate of Mars changed. Joel Davis deciphers the planet’s ancient, drying climate 14 DECEMBER 2020 | WWW.GEOLSOC.ORG.UK/GEOSCIENTIST WWW.GEOLSOC.ORG.UK/GEOSCIENTIST | DECEMBER 2020 | 15 FEATURE GEOSCIENTIST t has been an exciting year for Mars exploration. 2020 saw three spacecraft launches to the Red Planet, each by diff erent space agencies—NASA, the Chinese INational Space Administration, and the United Arab Emirates (UAE) Space Agency. NASA’s latest rover, Perseverance, is the fi rst step in a decade-long campaign for the eventual return of samples from Mars, which has the potential to truly transform our understanding of the still scientifi cally elusive Red Planet. On this side of the Atlantic, UK, European and Russian scientists are also getting ready for the launch of the European Space Agency (ESA) and Roscosmos Rosalind Franklin rover mission in 2022. The last 20 years have been a golden era for Mars exploration, with ever increasing amounts of data being returned from a variety of landed and orbital spacecraft. Such data help planetary geologists like me to unravel the complicated yet fascinating history of our celestial neighbour. As planetary geologists, we can apply our understanding of Earth to decipher the geological history of Mars, which is key to guiding future exploration. But why is planetary exploration so focused on Mars in particular? Until recently, the mantra of Mars exploration has been to follow the water, which has played an important role in shaping the surface of Mars.
    [Show full text]
  • Meyer, Michael Mars Exploration and Mars Sample Return
    Michael Meyer Lead Scientist Planetary Science Decadal Survey Mars Exploration & Mars Sample Return Panel on Mars, Nov 2, 2020 1 Why Mars? Mars is a habitable planet and has the potential to answer fundamental questions about our Solar System • The potential for life • A geological record of the first billion years of planetary evolution • A drastically changing climate through time • A compelling target for Human Exploration Mars Exploration Program Analysis Group Goals Human Life Climate Geology Exploration I. Determine if Mars ever supported life III. Understand II. Understand the origin and I. Determine if IV. Prepare for the processes evolution of Mars ever human and history of Mars as a supported, or exploration climate on Mars geological still supports life system Life I. Determine if Mars A. Search for evidence of life in environments that have a high potential for habitability and preservation of biosignatures. ever supported, or B. Assess the extent of abiotic organic chemical evolution. still supports, life. Climate II. Understand the A. Characterize the state and controlling processes of the present-day climate of Mars under the current orbital configuration. processes and B. Characterize the history and controlling processes of Mars’ climate in the recent past, history of climate under different orbital configurations. on Mars. C. Characterize Mars’ ancient climate and underlying processes. Geology III. Understand the A. Document the geologic record preserved in the crust and investigate the processes that have created and modified that record. origin and evolution B. Determine the structure, composition, and dynamics of the interior and how it has of Mars as a evolved.
    [Show full text]
  • GANGOTRI Mission Concept on the Glacial Key to the Amazonian Climate of Mars
    GANGOTRI mission concept on the glacial key to the Amazonian climate of Mars Coordinating authors: Suniti Karunatillake (legal last name: Walimuni Devage), Louisiana State University1 Ali Bramson, Purdue University Kris Zacny, Honeybee Robotics Colin Dundas, U.S. Geological Survey Lujendra Ojha, Rutgers University Corresponding author email address: [email protected] Endorsing: Science authors: 7 Paul Mahaffy Oded Aharonson, Planetary Science Institute Huiming Bao1 Eran Vos, Weizmann institute of science, Israel Jonathan Bapst5 Donald R. Hood, Texas A&M Deanne Rogers, Stony Brook University Joseph Levy, Colgate University Peter Doran1 Kathleen Mandt, JHU APL2 Jack Wilson2 Emily B. Hughes1, Wesleyan University Heidi Fuqua-Haviland, NASA-Marshall Space Flight Center3 Jeff Moersch, University of Tennessee, Knoxville Scott M. Perl, Jet Propulsion Laboratory5 Dewan Mohammad Enamul Haque1, University of Dhaka J.R. Skok, SETI Institute Harish, Physical Research Laboratory, India4 Vijayan S.4 Anil Bhardwaj4 Brent Christner, University of Florida Hanna Sizemore, Planetary Science Institute Akos Kereszturi, Research Centre for Astronomy and Earth Sciences, Hungary Norbert Schorghofer, Planetary Science Institute Kurt Retherford, South West Research Institute Paul Niles Johnson Space Center Technology development authors: , Juan Lorenzo1 Katherine Mesick, Los Alamos National Laboratory6 Heather Franz, Goddard Space Flight Center7 Jose Rodriguez-Manfredi, Centro de Astrobiologia INTA-CSIC, Spain Daniel Coupland6 Nathan Bramall, Leiden Measurement Technology Peter Bertone3 Cover Images: Harish et al. (2020) 10.1029/2020GL089057, excerpts copyright approved by Geophys. Res. Lett. on 08/04/2020 GANGOTRI mission concept Motivation and overview. The wealth of geologic information bound in Martian ice, including climate cycles, potential biomarkers, atmospheric particulates, and sources of H2O that may drive alteration within the critical zone (CZ: zone of interaction between the atmosphere and the porous upper crust) has long been recognized.
    [Show full text]
  • The Case for Rainfall on a Warm, Wet Early Mars Robert A
    JOURNAL OF GEOPHYSICAL RESEARCH, VOL. 107, NO. E11, 5111, doi:10.1029/2001JE001505, 2002 The case for rainfall on a warm, wet early Mars Robert A. Craddock Center for Earth and Planetary Studies, National Air and Space Museum, Smithsonian Institution, Washington, District of Columbia, USA Alan D. Howard Department of Environmental Sciences, University of Virginia, Charlottesville, Virginia, USA Received 11 April 2001; revised 10 April 2002; accepted 10 June 2002; published 23 November 2002. [1] Valley networks provide compelling evidence that past geologic processes on Mars were different than those seen today. The generally accepted paradigm is that these features formed from groundwater circulation, which may have been driven by differential heating induced by magmatic intrusions, impact melt, or a higher primordial heat flux. Although such mechanisms may not require climatic conditions any different than today’s, they fail to explain the large amount of recharge necessary for maintaining valley network systems, the spatial patterns of erosion, or how water became initially situated in the Martian regolith. In addition, there are no clear surface manifestations of any geothermal systems (e.g., mineral deposits or phreatic explosion craters). Finally, these models do not explain the style and amount of crater degradation. To the contrary, analyses of degraded crater morphometry indicate modification occurred from creep induced by rain splash combined with surface runoff and erosion; the former process appears to have continued late into Martian history. A critical analysis of the morphology and drainage density of valley networks based on Mars Global Surveyor data shows that these features are, in fact, entirely consistent with rainfall and surface runoff.
    [Show full text]
  • MAVEN Mars Atmosphere and Volatile Evolution Mission
    MAVEN Mars Atmosphere and Volatile Evolution Mission The Mars Atmosphere and Volatile Evolution Mission (MAVEN), launched on November 18, 2013, will explore the planet’s upper atmosphere, ionosphere, (Courtesy NASA/GSFC) and interactions with the Sun and solar wind. Frequently Asked Questions Quick Facts What is the purpose of MAVEN? Launch date: Nov. 18, 2013 Launch location: Cape Canaveral Air Force Station, Florida MAVEN is the first spacecraft that will focus primarily on the Launch vehicle: Atlas V-401 state of the upper atmosphere of Mars, the processes that control Mission target: Mars it, and the overall atmospheric loss that is currently occurring. Primary duration: One Earth year after arrival at Mars Specifically, MAVEN will explore the processes through which the Project description: Led by Principal Investigator Bruce top of the Martian atmosphere can be lost to space. Scientists think Jakosky of LASP, MAVEN is a NASA Mars Scout mission that this loss could be important in explaining the changes in the carrying eight instruments designed to orbit Mars and climate of Mars that have occurred over the last four billion years. explore its upper atmosphere. LASP provides: Why is climate change important on Mars? • The Imaging Ultraviolet Spectrometer (IUVS) instrument The present Mars atmosphere is composed almost entirely of • The Langmuir Probe and Waves (LPW) instrument CO2 and is about 1% as thick as the Earth’s atmosphere; surface • Science operations and data center temperatures average about 50°C below the freezing point of • Education and public outreach (EPO) water. However, evidence suggests that this was not always the Other organizations involved: case.
    [Show full text]
  • Moon-Miners-Manifesto-Mars.Pdf
    http://www.moonsociety.org/mars/ Let’s make the right choice - Mars and the Moon! Advantages of a low profile for shielding Mars looks like Arizona but feels like Antarctica Rover Opportunity at edge of Endeavor Crater Designing railroads and trains for Mars Designing planes that can fly in Mars’ thin air Breeding plants to be “Mars-hardy” Outposts between dunes, pulling sand over them These are just a few of the Mars-related topics covered in the past 25+ years. Read on for much more! Why Mars? The lunar and Martian frontiers will thrive much better as trading partners than either could on it own. Mars has little to trade to Earth, but a lot it can trade with the Moon. Both can/will thrive together! CHRONOLOGICAL INDEX MMM THEMES: MARS MMM #6 - "M" is for Missing Volatiles: Methane and 'Mmonia; Mars, PHOBOS, Deimos; Mars as I see it; MMM #16 Frontiers Have Rough Edges MMM #18 Importance of the M.U.S.-c.l.e.Plan for the Opening of Mars; Pavonis Mons MMM #19 Seizing the Reins of the Mars Bandwagon; Mars: Option to Stay; Mars Calendar MMM #30 NIMF: Nuclear rocket using Indigenous Martian Fuel; Wanted: Split personality types for Mars Expedition; Mars Calendar Postscript; Are there Meteor Showers on Mars? MMM #41 Imagineering Mars Rovers; Rethink Mars Sample Return; Lunar Development & Mars; Temptations to Eco-carelessness; The Romantic Touch of Old Barsoom MMM #42 Igloos: Atmosphere-derived shielding for lo-rem Martian Shelters MMM #54 Mars of Lore vs. Mars of Yore; vendors wanted for wheeled and walking Mars Rovers; Transforming Mars; Xities
    [Show full text]
  • Mars Atmosphere History and Surface Interactions
    Mars Atmosphere History and Surface Interactions David C. Catling University of Bristol, Bristol, United Kingdom University of Washington, Seattle, Washington Conway Leovy University of Washington, Seattle, Washington Cite: DC Catling, C Leovy, in Encyclopedia of the Solar CHAPTER 15 System (Ed. L McFadden, P Weissman), Academic Press, p.301-314, 2006. 1. Introduction Concluding Remarks 2. Volatile Inventories and their History Bibliography 3. Present and Past Climates fundamental question about the surface of Mars is But the present climate does not favor liquid water near A whether it was ever conducive to life in the past, which the surface. Surface temperatures range from about 140 ◦ is related to the broader questions of how the planet’s at- to 310 K. Above freezing temperatures occur only under mosphere evolved over time and whether past climates highly desiccating conditions in a thin layer at the interface supported widespread liquid water. Taken together, geo- between soil and atmosphere, and surface pressure over chemical data and models support the view that much of much of the planet is below the triple point of water [611 the original atmospheric inventory was lost to space before Pascals or 6.11 millibars (mbar)]. If liquid water is present about 3.5 billion years ago. It is widely believed that be- near the surface of Mars today, it must be confined to thin fore this time the climate would have needed to be warmer adsorbed layers on soil particles or highly saline solutions. in order to produce certain geological features, particularly No standing or flowing liquid water, saline or otherwise, has valley networks, but exactly how the early atmosphere pro- been found.
    [Show full text]
  • The Present and Past Climates of Planet Mars
    Eur. Phys. J. Conferences 1, 235–248 (2009) c EDP Sciences, 2009 THE EUROPEAN DOI: 10.1140/epjconf/e2009-0924-9 PHYSICAL JOURNAL CONFERENCES The present and past climates of planet Mars F. Forget LaboratoiredeM´et´eorologie Dynamique, IPSL, CNRS, Universit´e Paris 6, BP. 99, 75005 Paris, France Abstract. Mars is a small planet with a thin atmosphere of almost pure carbon dioxide. To first order, the Martian meteorology can be compared with what one would expect on a cold, dry desert-like Earth. However, several phenomena make the Martian climate system more complex than it appears. First, as much as 30% of the carbon dioxide atmosphere condenses every winter at high latitude to form CO2 ice polar caps, inducing large surface pressure variations all over the planet and an atmospheric circulation without equivalent on Earth. Second, a highly variable amount of suspended dust lifted by the winds modifies the radiative properties of the atmosphere, with sometime global dust storms able to totally shroud the planet. Last, a peculiar water cycle occurs on Mars, with water vapor transported by the atmosphere between the polar caps and possibly subsurface reservoirs, allowing the formation of clouds, hazes and frost. Telescopic and spacecraft observations have shown us that this complex climate system is highly variable, seasonally and from year to year, but these variations remain poorly understood. In fact, the Martian climate system has probably experienced large variations related to the oscillations in the parameters of the orbit and rotation of Mars (obliquity) a few millions or even thousand of years ago.
    [Show full text]
  • Effects of Global and Regional Dust Storms on the Martian Hot O Corona And
    Lee Yuni (Orcid ID: 0000-0003-0463-7650) Fang Xiaohua (Orcid ID: 0000-0002-6584-2837) Gacesa Marko (Orcid ID: 0000-0001-5145-051X) Ma Ying Juan (Orcid ID: 0000-0003-2584-7091) Mahaffy Paul, R. (Orcid ID: 0000-0003-1896-1726) Dong Chuanfei (Orcid ID: 0000-0002-8990-094X) Combi Michael R. (Orcid ID: 0000-0002-9805-0078) Bougher Stephen, W. (Orcid ID: 0000-0002-4178-2729) Jakosky Bruce, M. (Orcid ID: 0000-0002-0758-9976) Effects of Global and Regional Dust Storms on the Martian Hot O Corona and Photochemical Loss Yuni Lee1,2, Xiaohua Fang3, Marko Gacesa4,5, Yingjuan Ma6, Valeriy Tenishev7, Paul Mahaffy1, Chuanfei Dong8, Michael Combi7, Stephen Bougher7, and Bruce Jakosky3 1NASA Goddard Space Flight Center, USA 2University of Maryland Baltimore County, CRESST II, USA 3Laboratory for Atmospheric and Space Physics, University of Colorado Boulder, USA 4Space Science Division, NASA Ames Research Center, Moffett Field, California, USA 5Bay Area Environmental Research Institute (BAERI), Moffett Field, California, USA 6Department of Earth, Planetary, and Space Sciences, University of California, Los Angeles, USA 7Climate and Space Sciences and Engineering Department, University of Michigan, Ann Arbor, MI, USA 8Department of Astrophysical Sciences and Princeton Plasma Physics Laboratory, Princeton University, Princeton, NJ, USA *Corresponding author: [email protected] Key points: This is the author manuscript accepted for publication and has undergone full peer review but has not been through the copyediting, typesetting, pagination and proofreading process, which may lead to differences between this version and the Version of Record. Please cite this article as doi: 10.1029/2019JA027115 This article is protected by copyright.
    [Show full text]