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Ansari S, Kite ES, Ramirez R, Steele LJ, Mohseni H. Feasibility of keeping Mars warm with nanoparticles. SCIENCE ADVANCES 2024; 10:eadn4650. [PMID: 39110809 PMCID: PMC11305381 DOI: 10.1126/sciadv.adn4650] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Figures] [Subscribe] [Scholar Register] [Received: 12/11/2023] [Accepted: 07/09/2024] [Indexed: 08/10/2024]
Abstract
One-third of Mars' surface has shallow-buried H2O, but it is currently too cold for use by life. Proposals to warm Mars using greenhouse gases require a large mass of ingredients that are rare on Mars' surface. However, we show here that artificial aerosols made from materials that are readily available at Mars-for example, conductive nanorods that are ~9 micrometers long-could warm Mars >5 × 103 time smore effectively than the best gases. Such nanoparticles forward-scatter sunlight and efficiently block upwelling thermal infrared. Like the natural dust of Mars, they are swept high into Mars' atmosphere, allowing delivery from the near-surface. For a 10-year particle lifetime, two climate models indicate that sustained release at 30 liters per second would globally warm Mars by ≳30 kelvin and start to melt the ice. Therefore, if nanoparticles can be made at scale on (or delivered to) Mars, then the barrier to warming of Mars appears to be less high than previously thought.
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Affiliation(s)
- Samaneh Ansari
- Department of Electrical and Computer Engineering, Northwestern University, Evanston, IL, USA
| | - Edwin S. Kite
- Department of the Geophysical Sciences, University of Chicago, Chicago, IL, USA
| | - Ramses Ramirez
- Department of Physics, University of Central Florida, Orlando, FL, USA
| | - Liam J. Steele
- Department of the Geophysical Sciences, University of Chicago, Chicago, IL, USA
- European Center for Medium-Range Weather Forecasts, Reading, UK
| | - Hooman Mohseni
- Department of Electrical and Computer Engineering, Northwestern University, Evanston, IL, USA
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2
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Love R, Jackson DWT, Michaels T, Smyth TAG, Avouac JP, Cooper A. From Macro- to Microscale: A combined modelling approach for near-surface wind flow on Mars at sub-dune length-scales. PLoS One 2022; 17:e0276547. [PMCID: PMC9635718 DOI: 10.1371/journal.pone.0276547] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 08/15/2022] [Accepted: 10/07/2022] [Indexed: 11/06/2022] Open
Abstract
The processes that initiate and sustain sediment transport which contribute to the modification of aeolian deposits in Mars’ low-density atmosphere are still not fully understood despite recent atmospheric modelling. However, detailed microscale wind flow modelling, using Computational Fluid Dynamics at a resolution of <2 m, provides insights into the near-surface processes that cannot be modeled using larger-scale atmospheric modeling. Such Computational Fluid Dynamics simulations cannot by themselves account for regional-scale atmospheric circulations or flow modifications induced by regional km-scale topography, although realistic fine-scale mesoscale atmospheric modeling can. Using the output parameters from mesoscale simulations to inform the input conditions for the Computational Fluid Dynamics microscale simulations provides a practical approach to simulate near-surface wind flow and its relationship to very small-scale topographic features on Mars, particularly in areas which lack in situ rover data. This paper sets out a series of integrated techniques to enable a multi-scale modelling approach for surface airflow to derive surface airflow dynamics at a (dune) landform scale using High Resolution Imaging Science Experiment derived topographic data. The work therefore provides a more informed and realistic Computational Fluid Dynamics microscale modelling method, which will provide more detailed insight into the surface wind forcing of aeolian transport patterns on martian surfaces such as dunes.
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Affiliation(s)
- Richard Love
- School of Geography & Environmental Sciences, Ulster University, Northern Ireland, United Kingdom
- * E-mail:
| | - Derek W. T. Jackson
- School of Geography & Environmental Sciences, Ulster University, Northern Ireland, United Kingdom
- Geological Sciences, University of KwaZulu-Natal, Durban, South Africa
| | - Timothy Michaels
- Carl Sagan Center (at the SETI Institute), Mountain View, California, United States of America
| | - Thomas A. G. Smyth
- Department of Biological and Geographical Sciences, School of Applied Sciences, University of Huddersfield, England, United Kingdom
| | - Jean-Philippe Avouac
- School of Geography & Environmental Sciences, Ulster University, Northern Ireland, United Kingdom
- Division of Geological and Planetary Sciences, CalTech, Pasadena, California, United States of America
| | - Andrew Cooper
- School of Geography & Environmental Sciences, Ulster University, Northern Ireland, United Kingdom
- Geological Sciences, University of KwaZulu-Natal, Durban, South Africa
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3
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Stack KM, Dietrich WE, Lamb MP, Sullivan RJ, Christian JR, Newman CE, O’Connell‐Cooper CD, Sneed JW, Day M, Baker M, Arvidson RE, Fedo CM, Khan S, Williams RME, Bennett KA, Bryk AB, Cofield S, Edgar LA, Fox VK, Fraeman AA, House CH, Rubin DM, Sun VZ, Van Beek JK. Orbital and In-Situ Investigation of Periodic Bedrock Ridges in Glen Torridon, Gale Crater, Mars. JOURNAL OF GEOPHYSICAL RESEARCH. PLANETS 2022; 127:e2021JE007096. [PMID: 35865672 PMCID: PMC9286800 DOI: 10.1029/2021je007096] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Key Words] [Track Full Text] [Download PDF] [Figures] [Subscribe] [Scholar Register] [Received: 10/18/2021] [Revised: 05/03/2022] [Accepted: 05/07/2022] [Indexed: 06/15/2023]
Abstract
Gale crater, the field site for NASA's Mars Science Laboratory Curiosity rover, contains a diverse and extensive record of aeolian deposition and erosion. This study focuses on a series of regularly spaced, curvilinear, and sometimes branching bedrock ridges that occur within the Glen Torridon region on the lower northwest flank of Aeolis Mons, the central mound within Gale crater. During Curiosity's exploration of Glen Torridon between sols ∼2300-3080, the rover drove through this field of ridges, providing the opportunity for in situ observation of these features. This study uses orbiter and rover data to characterize ridge morphology, spatial distribution, compositional and material properties, and association with other aeolian features in the area. Based on these observations, we find that the Glen Torridon ridges are consistent with an origin as wind-eroded bedrock ridges, carved during the exhumation of Mount Sharp. Erosional features like the Glen Torridon ridges observed elsewhere on Mars, termed periodic bedrock ridges (PBRs), have been interpreted to form transverse to the dominant wind direction. The size and morphology of the Glen Torridon PBRs are consistent with transverse formative winds, but the orientation of nearby aeolian bedforms and bedrock erosional features raise the possibility of PBR formation by a net northeasterly wind regime. Although several formation models for the Glen Torridon PBRs are still under consideration, and questions persist about the nature of PBR-forming paleowinds, the presence of PBRs at this site provides important constraints on the depositional and erosional history of Gale crater.
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Affiliation(s)
- Kathryn M. Stack
- Jet Propulsion LaboratoryCalifornia Institute of TechnologyPasadenaCAUSA
| | - William E. Dietrich
- Department of Earth and Planetary ScienceUniversity of California, BerkeleyBerkeleyCAUSA
| | - Michael P. Lamb
- Division of Geological and Planetary SciencesCalifornia Institute of TechnologyPasadenaCAUSA
| | - Robert J. Sullivan
- Cornell Center for Astrophysics & Planetary ScienceCornell UniversityIthacaNYUSA
| | - John R. Christian
- Department of Earth and Planetary SciencesWashington University in St. LouisSt. LouisMOUSA
| | | | | | - Jonathan W. Sneed
- Department of Earth, Planetary, and Space SciencesUniversity of California, Los AngelesLos AngelesCAUSA
| | - Mackenzie Day
- Department of Earth, Planetary, and Space SciencesUniversity of California, Los AngelesLos AngelesCAUSA
| | - Mariah Baker
- Center for Earth & Planetary StudiesNational Air & Space MuseumSmithsonian InstitutionWashingtonDCUSA
| | - Raymond E. Arvidson
- Department of Earth and Planetary SciencesWashington University in St. LouisSt. LouisMOUSA
| | - Christopher M. Fedo
- Department of Earth and Planetary SciencesUniversity of Tennessee, KnoxvilleKnoxvilleTNUSA
| | - Sabrina Khan
- Department of Earth, Atmospheric, and Planetary SciencesMassachusetts Institute of TechnologyCambridgeMAUSA
| | | | | | - Alexander B. Bryk
- Department of Earth and Planetary ScienceUniversity of California, BerkeleyBerkeleyCAUSA
| | - Shannon Cofield
- U.S. Department of the InteriorBureau of Ocean Energy ManagementWashingtonDCUSA
| | - Lauren A. Edgar
- Astrogeology Science CenterU.S. Geological SurveyFlagstaffAZUSA
| | - Valerie K. Fox
- Earth and Environmental SciencesUniversity of MinnesotaMinneapolisMNUSA
| | - Abigail A. Fraeman
- Jet Propulsion LaboratoryCalifornia Institute of TechnologyPasadenaCAUSA
| | | | - David M. Rubin
- Earth and Planetary SciencesUniversity of California, Santa CruzSanta CruzCAUSA
| | - Vivian Z. Sun
- Jet Propulsion LaboratoryCalifornia Institute of TechnologyPasadenaCAUSA
| | - Jason K. Van Beek
- Jet Propulsion LaboratoryCalifornia Institute of TechnologyPasadenaCAUSA
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4
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Newman CE, Hueso R, Lemmon MT, Munguira A, Vicente-Retortillo Á, Apestigue V, Martínez GM, Toledo D, Sullivan R, Herkenhoff KE, de la Torre Juárez M, Richardson MI, Stott AE, Murdoch N, Sanchez-Lavega A, Wolff MJ, Arruego I, Sebastián E, Navarro S, Gómez-Elvira J, Tamppari L, Viúdez-Moreiras D, Harri AM, Genzer M, Hieta M, Lorenz RD, Conrad P, Gómez F, McConnochie TH, Mimoun D, Tate C, Bertrand T, Bell JF, Maki JN, Rodriguez-Manfredi JA, Wiens RC, Chide B, Maurice S, Zorzano MP, Mora L, Baker MM, Banfield D, Pla-Garcia J, Beyssac O, Brown A, Clark B, Lepinette A, Montmessin F, Fischer E, Patel P, del Río-Gaztelurrutia T, Fouchet T, Francis R, Guzewich SD. The dynamic atmospheric and aeolian environment of Jezero crater, Mars. SCIENCE ADVANCES 2022; 8:eabn3783. [PMID: 35613267 PMCID: PMC9132482 DOI: 10.1126/sciadv.abn3783] [Citation(s) in RCA: 2] [Impact Index Per Article: 1.0] [Reference Citation Analysis] [Abstract] [Grants] [Track Full Text] [Download PDF] [Figures] [Subscribe] [Scholar Register] [Received: 11/22/2021] [Accepted: 04/08/2022] [Indexed: 06/15/2023]
Abstract
Despite the importance of sand and dust to Mars geomorphology, weather, and exploration, the processes that move sand and that raise dust to maintain Mars' ubiquitous dust haze and to produce dust storms have not been well quantified in situ, with missions lacking either the necessary sensors or a sufficiently active aeolian environment. Perseverance rover's novel environmental sensors and Jezero crater's dusty environment remedy this. In Perseverance's first 216 sols, four convective vortices raised dust locally, while, on average, four passed the rover daily, over 25% of which were significantly dusty ("dust devils"). More rarely, dust lifting by nonvortex wind gusts was produced by daytime convection cells advected over the crater by strong regional daytime upslope winds, which also control aeolian surface features. One such event covered 10 times more area than the largest dust devil, suggesting that dust devils and wind gusts could raise equal amounts of dust under nonstorm conditions.
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Affiliation(s)
| | | | | | | | | | | | - Germán M. Martínez
- Lunar and Planetary Institute, USRA, Houston, TX, USA
- University of Michigan, Ann Arbor, MI, USA
| | | | | | | | | | | | | | - Naomi Murdoch
- ISAE-SUPAERO, Université de Toulouse, Toulouse, France
| | | | | | | | | | | | | | - Leslie Tamppari
- Jet Propulsion Laboratory–California Institute of Technology, Pasadena, CA, USA
| | | | | | - Maria Genzer
- Finnish Meteorological Institute, Helsinki, Finland
| | - Maria Hieta
- Finnish Meteorological Institute, Helsinki, Finland
| | | | - Pan Conrad
- Carnegie Institution for Science, Washington, DC, USA
| | | | | | - David Mimoun
- ISAE-SUPAERO, Université de Toulouse, Toulouse, France
| | | | | | | | - Justin N. Maki
- Jet Propulsion Laboratory–California Institute of Technology, Pasadena, CA, USA
| | | | - Roger C. Wiens
- Los Alamos National Laboratory, Los Alamos, NM, USA
- Purdue University, West Lafayette, IN, USA
| | | | | | | | - Luis Mora
- Centro de Astrobiologia, INTA, Madrid, Spain
| | - Mariah M. Baker
- Smithsonian National Air and Space Museum, Washington, DC, USA
| | - Don Banfield
- Cornell University, Ithaca, NY, USA
- NASA Ames, Mountain View, CA, USA
| | - Jorge Pla-Garcia
- Space Science Institute, Boulder, CO, USA
- Centro de Astrobiologia, INTA, Madrid, Spain
| | | | | | - Ben Clark
- Space Science Institute, Boulder, CO, USA
| | | | | | | | - Priyaben Patel
- Jet Propulsion Laboratory–California Institute of Technology, Pasadena, CA, USA
- UCL, London, UK
| | | | | | - Raymond Francis
- Jet Propulsion Laboratory–California Institute of Technology, Pasadena, CA, USA
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5
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Kite ES, Mischna MA, Fan B, Morgan AM, Wilson SA, Richardson MI. Changing spatial distribution of water flow charts major change in Mars's greenhouse effect. SCIENCE ADVANCES 2022; 8:eabo5894. [PMID: 35613275 PMCID: PMC9132440 DOI: 10.1126/sciadv.abo5894] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Grants] [Track Full Text] [Download PDF] [Figures] [Subscribe] [Scholar Register] [Received: 02/14/2022] [Accepted: 03/31/2022] [Indexed: 06/15/2023]
Abstract
Early Mars had rivers, but the cause of Mars's wet-to-dry transition remains unknown. Past climate on Mars can be probed using the spatial distribution of climate-sensitive landforms. We analyzed global databases of water-worked landforms and identified changes in the spatial distribution of rivers over time. These changes are simply explained by comparison to a simplified meltwater model driven by an ensemble of global climate model simulations, as the result of ≳10 K global cooling, from global average surface temperature [Formula: see text] ≥ 268 K to [Formula: see text] ~ 258 K, due to a weaker greenhouse effect. In other words, river-forming climates on early Mars were warm and wet first, and cold and wet later. Unexpectedly, analysis of the greenhouse effect within our ensemble of global climate model simulations suggests that this shift was primarily driven by waning non-CO2 radiative forcing, and not changes in CO2 radiative forcing.
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Affiliation(s)
| | - Michael A. Mischna
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109, USA
| | - Bowen Fan
- University of Chicago, Chicago, IL 60637, USA
| | - Alexander M. Morgan
- Smithsonian Institution, Washington, DC 20002, USA
- Planetary Science Institute, Tucson, AZ 85719, USA
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Characteristics of Dust Devils in Two Pre-Selected Landing Regions of the Tianwen-1 Mission—Comparing Observations and Predictions Using Numerical Model. REMOTE SENSING 2022. [DOI: 10.3390/rs14092117] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 12/04/2022]
Abstract
The spatial and temporal distribution of dust devils (DDs) in the two pre-selected landing regions (ZA and ZB) of the Tianwen-1 mission in southern Utopia Planitia have been investigated by using images from the Context Camera (CTX) of the Mars Reconnaissance Orbiter (MRO). From the images of the regions in 8 Martian years, no DD was found in ZA, while 77 DDs were found in ZB. The observed DDs are mainly distributed in the northeastern part of ZB. The temporal variation in the observed DDs shows a prominent two-peak pattern in their local early spring and late summer. The size and height of the observed DDs have also been evaluated from the images, and they show a similar temporal variation as the occurrence. To investigate the possible conditions pertinent to these observed patterns of DD distribution, some analysis based on the thermodynamic theory of heat engines was performed using the output of the Mars climate model, MarsWRF. The spatial and temporal distribution of the simulated DDs are generally consistent with the observation, with significantly more DDs in ZB. Analysis of the model results suggests that the spatial distributions of the predicted DDs are mainly related to the distribution of sensible heat flux, which, in turn, is mainly determined by the surface-to-air temperature difference. The difference in DDs between ZA and ZB (more DDs in ZB) is dominated by the difference in sensible heat flux, which, in turn, is mainly related to the spatial variation of surface albedo.
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7
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Luo Y, Mischna MA, Lin JC, Fasoli B, Cai X, Yung YL. Mars Methane Sources in Northwestern Gale Crater Inferred From Back Trajectory Modeling. EARTH AND SPACE SCIENCE (HOBOKEN, N.J.) 2021; 8:e2021EA001915. [PMID: 35860450 PMCID: PMC9285602 DOI: 10.1029/2021ea001915] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Download PDF] [Figures] [Subscribe] [Scholar Register] [Received: 07/11/2021] [Revised: 10/26/2021] [Accepted: 10/27/2021] [Indexed: 06/15/2023]
Abstract
During its first seven years of operation, the Sample Analysis at Mars Tunable Laser Spectrometer (TLS) on board the Curiosity rover has detected seven methane spikes above a low background abundance in Gale crater. The methane spikes are likely sourced by surface emission within or around Gale crater. Here, we use inverse Lagrangian modeling techniques to identify upstream emission regions on the Martian surface for these methane spikes at an unprecedented spatial resolution. Inside Gale crater, the northwestern crater floor casts the strongest influence on the detections. Outside Gale crater, the upstream regions common to all the methane spikes extend toward the north. The contrasting results from two consecutive TLS methane measurements performed on the same sol point to an active emission site to the west or the southwest of the Curiosity rover on the northwestern crater floor. The observed spike magnitude and frequency also favor emission sites on the northwestern crater floor, unless there are fast methane removal mechanisms at work, or either the methane spikes of TLS or the non-detections of ExoMars Trace Gas Orbiter cannot be trusted.
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Affiliation(s)
- Y. Luo
- Division of Geological and Planetary SciencesCalifornia Institute of TechnologyPasadenaCAUSA
| | - M. A. Mischna
- Jet Propulsion LaboratoryCalifornia Institute of TechnologyPasadenaCAUSA
| | - J. C. Lin
- Department of Atmospheric SciencesUniversity of UtahSalt Lake CityUTUSA
| | - B. Fasoli
- Department of Atmospheric SciencesUniversity of UtahSalt Lake CityUTUSA
| | - X. Cai
- Columbia UniversityNew YorkNYUSA
| | - Y. L. Yung
- Division of Geological and Planetary SciencesCalifornia Institute of TechnologyPasadenaCAUSA
- Jet Propulsion LaboratoryCalifornia Institute of TechnologyPasadenaCAUSA
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8
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Adams D, Luo Y, Wong ML, Dunn P, Christensen M, Dong C, Hu R, Yung Y. Nitrogen Fixation at Early Mars. ASTROBIOLOGY 2021; 21:968-980. [PMID: 34339294 DOI: 10.1089/ast.2020.2273] [Citation(s) in RCA: 3] [Impact Index Per Article: 1.0] [Reference Citation Analysis] [Abstract] [Key Words] [MESH Headings] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 06/13/2023]
Abstract
The Mars Science Laboratory (MSL) recently discovered nitrates in Gale Crater (e.g., Stern et al., 2015; Sutter et al., 2017). One possible mechanism for ancient nitrate deposition on Mars is through HNOx formation and rain out in the atmosphere, for which lightning-induced NO is likely the fundamental source. This study investigates nitrogen (N2) fixation in early Mars' atmosphere, with implications for early Mars' habitability. We consider a 1 bar atmosphere of background CO2, with abundance of N2, hydrogen, and methane varied from 1% to 10% to explore a swath of potential early Mars climates. We derive lightning-induced thermochemical equilibrium fluxes of NO and HCN by coupling the lightning-rate parametrization from the study of Romps et al. (2014) with chemical equilibrium with applications, and we use a Geant4 simulation platform to estimate the effect of solar energetic particle events. These fluxes are used as input into KINETICS, the Caltech/JPL coupled photochemistry and transport code, which models the chemistry of 50 species linked by 495 reactions to derive rain-out fluxes of HNOx and HCN. We compute equilibrium concentrations of cyanide and nitrate in a putative northern ocean at early Mars, assuming hydrothermal vent circulation and photoreduction act as the dominant loss mechanisms. We find average oceanic concentrations of ∼0.1-2 nM nitrate and ∼0.01-2 mM cyanide. HCN is critical for protein synthesis at concentrations >0.01 M (e.g., Holm and Neubeck, 2009), and our result is astrobiologically significant if secondary local concentration mechanisms occurred. Nitrates may act as high-potential electron acceptors for early metabolisms, although the minimum concentration required is unknown. Our study derives concentrations that will be useful for future laboratory studies to investigate the habitability at early Mars. The aqueous nitrate concentrations correspond to surface nitrate precipitates of ∼1-8 × 10-4 wt % that may have formed after the evaporation of surface waters, and these values roughly agree with recent MSL measurements.
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Affiliation(s)
- Danica Adams
- Department of Geological and Planetary Sciences, California Institute of Technology, Pasadena, California, USA
| | - Yangcheng Luo
- Department of Geological and Planetary Sciences, California Institute of Technology, Pasadena, California, USA
| | - Michael L Wong
- Department of Astronomy and Astrobiology Program, University of Washington, Seattle, Washington, USA
- Virtual Planet Laboratory, University of Washington, Seattle, Washington, USA
| | - Patrick Dunn
- Space Sciences Laboratory, University of California, Berkeley, Berkeley, California, USA
| | - Madeline Christensen
- Department of Geological and Planetary Sciences, California Institute of Technology, Pasadena, California, USA
- Bellarmine Preparatory, Tacoma, Washington, USA
| | - Chuanfei Dong
- Department of Astrophysical Sciences, Princeton University, Princeton, California, USA
| | - Renyu Hu
- Department of Geological and Planetary Sciences, California Institute of Technology, Pasadena, California, USA
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, California, USA
| | - Yuk Yung
- Department of Geological and Planetary Sciences, California Institute of Technology, Pasadena, California, USA
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, California, USA
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9
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Kite ES, Steele LJ, Mischna MA, Richardson MI. Warm early Mars surface enabled by high-altitude water ice clouds. Proc Natl Acad Sci U S A 2021; 118:e2101959118. [PMID: 33903256 PMCID: PMC8106349 DOI: 10.1073/pnas.2101959118] [Citation(s) in RCA: 7] [Impact Index Per Article: 2.3] [Reference Citation Analysis] [Abstract] [Key Words] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/18/2022] Open
Abstract
Despite receiving just 30% of the Earth's present-day insolation, Mars had water lakes and rivers early in the planet's history, due to an unknown warming mechanism. A possible explanation for the >102-y-long lake-forming climates is warming by water ice clouds. However, this suggested cloud greenhouse explanation has proved difficult to replicate and has been argued to require unrealistically optically thick clouds at high altitudes. Here, we use a global climate model (GCM) to show that a cloud greenhouse can warm a Mars-like planet to global average annual-mean temperature ([Formula: see text]) ∼265 K, which is warm enough for low-latitude lakes, and stay warm for centuries or longer, but only if the planet has spatially patchy surface water sources. Warm, stable climates involve surface ice (and low clouds) only at locations much colder than the average surface temperature. At locations horizontally distant from these surface cold traps, clouds are found only at high altitudes, which maximizes warming. Radiatively significant clouds persist because ice particles sublimate as they fall, moistening the subcloud layer so that modest updrafts can sustain relatively large amounts of cloud. The resulting climates are arid (area-averaged surface relative humidity ∼25%). In a warm, arid climate, lakes could be fed by groundwater upwelling, or by melting of ice following a cold-to-warm transition. Our results are consistent with the warm and arid climate favored by interpretation of geologic data, and support the cloud greenhouse hypothesis.
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Affiliation(s)
- Edwin S Kite
- Department of the Geophysical Sciences, University of Chicago, Chicago, IL 60615;
| | - Liam J Steele
- Department of the Geophysical Sciences, University of Chicago, Chicago, IL 60615
| | - Michael A Mischna
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109
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Newman CE, de la Torre Juárez M, Pla-García J, Wilson RJ, Lewis SR, Neary L, Kahre MA, Forget F, Spiga A, Richardson MI, Daerden F, Bertrand T, Viúdez-Moreiras D, Sullivan R, Sánchez-Lavega A, Chide B, Rodriguez-Manfredi JA. Multi-model Meteorological and Aeolian Predictions for Mars 2020 and the Jezero Crater Region. SPACE SCIENCE REVIEWS 2021; 217:20. [PMID: 33583960 PMCID: PMC7868679 DOI: 10.1007/s11214-020-00788-2] [Citation(s) in RCA: 6] [Impact Index Per Article: 2.0] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Received: 05/20/2020] [Accepted: 12/26/2020] [Indexed: 05/27/2023]
Abstract
UNLABELLED Nine simulations are used to predict the meteorology and aeolian activity of the Mars 2020 landing site region. Predicted seasonal variations of pressure and surface and atmospheric temperature generally agree. Minimum and maximum pressure is predicted at Ls ∼ 145 ∘ and 250 ∘ , respectively. Maximum and minimum surface and atmospheric temperature are predicted at Ls ∼ 180 ∘ and 270 ∘ , respectively; i.e., are warmest at northern fall equinox not summer solstice. Daily pressure cycles vary more between simulations, possibly due to differences in atmospheric dust distributions. Jezero crater sits inside and close to the NW rim of the huge Isidis basin, whose daytime upslope (∼east-southeasterly) and nighttime downslope (∼northwesterly) winds are predicted to dominate except around summer solstice, when the global circulation produces more southerly wind directions. Wind predictions vary hugely, with annual maximum speeds varying from 11 to 19 ms - 1 and daily mean wind speeds peaking in the first half of summer for most simulations but in the second half of the year for two. Most simulations predict net annual sand transport toward the WNW, which is generally consistent with aeolian observations, and peak sand fluxes in the first half of summer, with the weakest fluxes around winter solstice due to opposition between the global circulation and daytime upslope winds. However, one simulation predicts transport toward the NW, while another predicts fluxes peaking later and transport toward the WSW. Vortex activity is predicted to peak in summer and dip around winter solstice, and to be greater than at InSight and much greater than in Gale crater. SUPPLEMENTARY INFORMATION The online version contains supplementary material available at 10.1007/s11214-020-00788-2.
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Affiliation(s)
| | - M. de la Torre Juárez
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91001 USA
| | - J. Pla-García
- Centro de Astrobiología (CSIC-INTA), 28850 Madrid, Spain
- Space Science Institute, Boulder, CO 80301 USA
| | | | | | - L. Neary
- Belgian Institute for Space Aeronomy, Brussels, Belgium
| | | | - F. Forget
- Laboratoire de Météorologie Dynamique/Institut Pierre Simon Laplace (LMD/IPSL), Sorbonne Université, Centre National de la Recherche Scientifique (CNRS), École Polytechnique, École Normale Supérieure (ENS), 75005 Paris, France
| | - A. Spiga
- Laboratoire de Météorologie Dynamique/Institut Pierre Simon Laplace (LMD/IPSL), Sorbonne Université, Centre National de la Recherche Scientifique (CNRS), École Polytechnique, École Normale Supérieure (ENS), 75005 Paris, France
- Institut Universitaire de France, 75005 Paris, France
| | | | - F. Daerden
- Belgian Institute for Space Aeronomy, Brussels, Belgium
| | - T. Bertrand
- Ames Research Center, Mountain View, CA USA
- LESIA, Observatoire de Paris, Université PSL, CNRS, Sorbonne Université, Université de Paris, 92195 Meudon, France
| | | | - R. Sullivan
- Cornell Center for Astrophysics and Planetary Science, Cornell University, Ithaca, NY 14853 USA
| | | | - B. Chide
- Institut Supérieur de l’Aéronautique et de l’Espace (ISAE), Toulouse, France
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11
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Baumgartner M, Weigel R, Harvey AH, Plöger F, Achatz U, Spichtinger P. Reappraising the appropriate calculation of a common meteorological quantity: Potential Temperature. ATMOSPHERIC CHEMISTRY AND PHYSICS 2020; 20:10.5194/acp-20-15585-2020. [PMID: 34093695 PMCID: PMC8174307 DOI: 10.5194/acp-20-15585-2020] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 06/12/2023]
Abstract
The potential temperature is a widely used quantity in atmospheric science since it is conserved for dry air's adiabatic changes of state. Its definition involves the specific heat capacity of dry air, which is traditionally assumed as constant. However, the literature provides different values of this allegedly constant parameter, which are reviewed and discussed in this study. Furthermore, we derive the potential temperature for a temperature-dependent parameterisation of the specific heat capacity of dry air, thus providing a new reference potential temperature with a more rigorous basis. This new reference shows different values and vertical gradients, in particular in the stratosphere and above, compared to the potential temperature that assumes constant heat capacity. The application of the new reference potential temperature is discussed for computations of the Brunt-Väisälä frequency, Ertel's potential vorticity, diabatic heating rates, and for the vertical sorting of observational data.
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Affiliation(s)
- Manuel Baumgartner
- Zentrum für Datenverarbeitung, Johannes Gutenberg University Mainz, Germany
- Institute for Atmospheric Physics, Johannes Gutenberg University Mainz, Germany
| | - Ralf Weigel
- Institute for Atmospheric Physics, Johannes Gutenberg University Mainz, Germany
| | - Allan H. Harvey
- Applied Chemicals and Materials Division, National Institute of Standards and Technology, Boulder, CO, USA
| | - Felix Plöger
- Forschungszentrum Jülich GmbH, Institute of Energy and Climate Research (IEK-7), Jülich, Germany
- Institute for Atmospheric and Environmental Research, University of Wuppertal, Wuppertal, Germany
| | - Ulrich Achatz
- Institut für Atmosphäre und Umwelt, Goethe-Universität Frankfurt, Frankfurt am Main, Germany
| | - Peter Spichtinger
- Institute for Atmospheric Physics, Johannes Gutenberg University Mainz, Germany
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12
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Chevrier VF, Rivera-Valentín EG, Soto A, Altheide TS. Global Temporal and Geographic Stability of Brines on Present-day Mars. THE PLANETARY SCIENCE JOURNAL 2020; 1:64. [PMID: 34647027 PMCID: PMC8507180 DOI: 10.3847/psj/abbc14] [Citation(s) in RCA: 3] [Impact Index Per Article: 0.8] [Reference Citation Analysis] [Abstract] [Grants] [Track Full Text] [Figures] [Subscribe] [Scholar Register] [Indexed: 06/13/2023]
Abstract
We combine experimentally verified constraints on brine thermodynamics along with a global circulation model to develop a new extensive framework of brine stability on the surface and subsurface of Mars. Our work considers all major phase changes (i.e., evaporation, freezing, and boiling) and is consistent, regardless of brine composition, so it is applicable to any brine relevant to Mars. We find that equatorial regions typically have temperatures too high for stable brines, while high latitudes are susceptible to permanent freezing. In the subsurface, this trend is reversed, and equatorial regions are more favorable to brine stability, but only for the lowest water activities (and lowest eutectic temperatures). At locations where brines may be stable, we find that their lifetimes can be characterized by two regimes. Above a water activity of ~0.6, brine duration is dominated by evaporation, lasting at most a few minutes per sol. Below a water activity of 0.6, brine duration is bound by freezing or boiling; such brines are potentially stable for up to several consecutive hours per sol. Our work suggests that brines should not be expected near or on the Martian surface, except for low eutectic water activity salts such as calcium or magnesium perchlorate or chlorate, and their (meta)stability on the surface would require contact with atmospheric water vapor or local ice deposits.
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Affiliation(s)
- Vincent F Chevrier
- Arkansas Center for Space and Planetary Sciences, University of Arkansas, Fayetteville, AR 72701, USA
| | | | | | - Travis S Altheide
- Department of Medical Laboratory Science, Eastern Kentucky University, 219 Dizney Building, 521 Lancaster Avenue, Richmond, KY 40475, USA
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Breuer H, Berényi A, Mari L, Nagy B, Szalai Z, Tordai Á, Weidinger T. Analog Site Experiment in the High Andes-Atacama Region: Surface Energy Budget Components on Ojos del Salado from Field Measurements and WRF Simulations. ASTROBIOLOGY 2020; 20:684-700. [PMID: 32048870 DOI: 10.1089/ast.2019.2024] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Key Words] [MESH Headings] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 06/10/2023]
Abstract
Remote sensing data are abundant, whereas surface in situ verification of atmospheric conditions is rare on Mars. Earth-based analogs could help gain an understanding of soil and atmospheric processes on Mars and refine existing models. In this work, we evaluate the applicability of the Weather Research and Forecasting (WRF) model against measurements from the Mars analog High Andes-Atacama Desert. Validation focuses on the surface conditions and on the surface energy budget. Measurements show that the average daily net radiation, global radiation, and latent heat flux amount to 131, 273, and about 10 W/m2, respectively, indicating extremely dry atmospheric conditions. Dynamically, the effect of topography is also well simulated. One of the main modeling problems is the inaccurate initial soil and surface conditions in the area. Correction of soil moisture based on in situ and satellite soil moisture measurements, as well as the removal of snow coverage, reduced the surface skin temperature root mean square error from 9.8°C to 4.3°C. The model, however, has shortcomings when soil condition modeling is considered. Sensible heat flux estimations are on par with the measurements (daily maxima around 500 W/m2), but surface soil heat flux is greatly overestimated (by 150-500 W/m2). Soil temperature and soil moisture diurnal variations are inconsistent with the measurements, partially due to the lack of water vapor representation in soil calculations.
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Affiliation(s)
- Hajnalka Breuer
- Department of Meteorology, Eötvös Loránd University, Budapest, Hungary
| | - Alexandra Berényi
- Department of Meteorology, Eötvös Loránd University, Budapest, Hungary
| | - László Mari
- Department of Physical Geography, Eötvös Loránd University, Budapest, Hungary
| | - Balázs Nagy
- Department of Physical Geography, Eötvös Loránd University, Budapest, Hungary
| | - Zoltán Szalai
- Department of Environmental and Landscape Geography, Eötvös Loránd University, Budapest, Hungary
- Geographical Research Institute, Research Centre for Astronomy and Earth Sciences, Hungarian Academy of Sciences, Budapest, Hungary
| | - Ágoston Tordai
- Department of Meteorology, Eötvös Loránd University, Budapest, Hungary
| | - Tamás Weidinger
- Department of Meteorology, Eötvös Loránd University, Budapest, Hungary
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14
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The Mars Regional Atmospheric Modeling System (MRAMS): Current Status and Future Directions. ATMOSPHERE 2019. [DOI: 10.3390/atmos10120747] [Citation(s) in RCA: 12] [Impact Index Per Article: 2.4] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 01/30/2023]
Abstract
The Mars Regional Atmospheric Modeling System (MRAMS) is closing in on two decades of use as a tool to investigate mesoscale and microscale circulations and dynamics in the atmosphere of Mars. Over this period of time, there have been numerous improvements and additions to the model dynamical core, physical parameterizations, and framework. At the same time, the application of the model to Mars (and related code for other planets) has taught many lessons about limitations and cautions that should be exercised. The current state of MRAMS is described along with a review of prior studies and findings utilizing the model. Where appropriate, lessons learned are provided to help guide future users and aid in the design and interpretation of numerical experiments. The paper concludes with a discussion of future MRAMS development plans.
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Moore CA, Moores JE, Newman CE, Lemmon MT, Guzewich SD, Battalio M. Vertical and Horizontal Heterogeneity of Atmospheric Dust Loading in Northern Gale Crater, Mars. ICARUS 2019; 329:197-206. [PMID: 31359883 PMCID: PMC6662233 DOI: 10.1016/j.icarus.2019.03.041] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 06/10/2023]
Abstract
This paper updates the record of atmospheric dust loading within northern Gale Crater, Mars, by providing line-of-sight extinction (LOS-Ext) measurements of the intervening dust between the rover and the crater rim. These measurements are derived from images taken with the Navigation Cameras (Navcam) onboard the Mars Science Laboratory (MSL) rover, Curiosity. The observations span 2.44 Mars years, from Mars Year (MY) 31 at a solar longitude (L S ) of 208° to t L S = 7° of MY34, sols 100 - 1701 of the MSL surface mission. This work examines the dataset for seasonal trends of the LOS-Ext in addition to horizontal variations and the vertical structure of LOS-Ext. The LOS-Ext has a repetitive pattern with a single peak in the latter half of the Mars year. The atmosphere in the crater is well mixed horizontally but not vertically as larger LOS-Ext is seen nearer the crater floor than at higher altitudes within the crater. The results allow a discussion on whether or not Gale Crater is a sink for atmospheric dust or a source of atmospheric dust in the current era.
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Affiliation(s)
- Casey A Moore
- York University, Centre for Research in Earth and Space Sciences (CRESS), 4700 Keele Street, Toronto ON M3J 1P3, Canada
| | - John E Moores
- York University, Centre for Research in Earth and Space Sciences (CRESS), 4700 Keele Street, Toronto ON M3J 1P3, Canada
| | | | - Mark T Lemmon
- Texas A&M University, Department of Atmospheric Sciences, MS 3150 College Station, Texas 77843, United States
| | - Scott D Guzewich
- NASA Goddard Space Flight Center, Greenbelt, MD 20771, United States
| | - Michael Battalio
- Texas A&M University, Department of Atmospheric Sciences, MS 3150 College Station, Texas 77843, United States
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Yung YL, Chen P, Nealson K, Atreya S, Beckett P, Blank JG, Ehlmann B, Eiler J, Etiope G, Ferry JG, Forget F, Gao P, Hu R, Kleinböhl A, Klusman R, Lefèvre F, Miller C, Mischna M, Mumma M, Newman S, Oehler D, Okumura M, Oremland R, Orphan V, Popa R, Russell M, Shen L, Sherwood Lollar B, Staehle R, Stamenković V, Stolper D, Templeton A, Vandaele AC, Viscardy S, Webster CR, Wennberg PO, Wong ML, Worden J. Methane on Mars and Habitability: Challenges and Responses. ASTROBIOLOGY 2018; 18:1221-1242. [PMID: 30234380 PMCID: PMC6205098 DOI: 10.1089/ast.2018.1917] [Citation(s) in RCA: 4] [Impact Index Per Article: 0.7] [Reference Citation Analysis] [Abstract] [Key Words] [MESH Headings] [Track Full Text] [Subscribe] [Scholar Register] [Received: 06/07/2018] [Accepted: 06/12/2018] [Indexed: 05/05/2023]
Abstract
Recent measurements of methane (CH4) by the Mars Science Laboratory (MSL) now confront us with robust data that demand interpretation. Thus far, the MSL data have revealed a baseline level of CH4 (∼0.4 parts per billion by volume [ppbv]), with seasonal variations, as well as greatly enhanced spikes of CH4 with peak abundances of ∼7 ppbv. What do these CH4 revelations with drastically different abundances and temporal signatures represent in terms of interior geochemical processes, or is martian CH4 a biosignature? Discerning how CH4 generation occurs on Mars may shed light on the potential habitability of Mars. There is no evidence of life on the surface of Mars today, but microbes might reside beneath the surface. In this case, the carbon flux represented by CH4 would serve as a link between a putative subterranean biosphere on Mars and what we can measure above the surface. Alternatively, CH4 records modern geochemical activity. Here we ask the fundamental question: how active is Mars, geochemically and/or biologically? In this article, we examine geological, geochemical, and biogeochemical processes related to our overarching question. The martian atmosphere and surface are an overwhelmingly oxidizing environment, and life requires pairing of electron donors and electron acceptors, that is, redox gradients, as an essential source of energy. Therefore, a fundamental and critical question regarding the possibility of life on Mars is, "Where can we find redox gradients as energy sources for life on Mars?" Hence, regardless of the pathway that generates CH4 on Mars, the presence of CH4, a reduced species in an oxidant-rich environment, suggests the possibility of redox gradients supporting life and habitability on Mars. Recent missions such as ExoMars Trace Gas Orbiter may provide mapping of the global distribution of CH4. To discriminate between abiotic and biotic sources of CH4 on Mars, future studies should use a series of diagnostic geochemical analyses, preferably performed below the ground or at the ground/atmosphere interface, including measurements of CH4 isotopes, methane/ethane ratios, H2 gas concentration, and species such as acetic acid. Advances in the fields of Mars exploration and instrumentation will be driven, augmented, and supported by an improved understanding of atmospheric chemistry and dynamics, deep subsurface biogeochemistry, astrobiology, planetary geology, and geophysics. Future Mars exploration programs will have to expand the integration of complementary areas of expertise to generate synergistic and innovative ideas to realize breakthroughs in advancing our understanding of the potential of life and habitable conditions having existed on Mars. In this spirit, we conducted a set of interdisciplinary workshops. From this series has emerged a vision of technological, theoretical, and methodological innovations to explore the martian subsurface and to enhance spatial tracking of key volatiles, such as CH4.
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Affiliation(s)
- Yuk L. Yung
- California Institute of Technology, Pasadena, California
- NASA Jet Propulsion Laboratory, California Institute of Technology, Pasadena, California
| | - Pin Chen
- NASA Jet Propulsion Laboratory, California Institute of Technology, Pasadena, California
| | | | | | | | - Jennifer G. Blank
- NASA Ames Research Center, Blue Marble Space Institute of Science, Mountain View, California
| | - Bethany Ehlmann
- California Institute of Technology, Pasadena, California
- NASA Jet Propulsion Laboratory, California Institute of Technology, Pasadena, California
| | - John Eiler
- California Institute of Technology, Pasadena, California
| | - Giuseppe Etiope
- Istituto Nazionale di Geofisica e Vulcanologia, Rome, Italy
- Faculty of Environmental Science and Engineering, Babes-Bolyai University, Cluj-Napoca, Romania
| | - James G. Ferry
- The Pennsylvania State University, University Park, Pennsylvania
| | - Francois Forget
- Laboratoire de Météorologie Dynamique, Institut Pierre Simon Laplace, CNRS, Paris, France
| | - Peter Gao
- University of California, Berkeley, California
| | - Renyu Hu
- NASA Jet Propulsion Laboratory, California Institute of Technology, Pasadena, California
| | - Armin Kleinböhl
- NASA Jet Propulsion Laboratory, California Institute of Technology, Pasadena, California
| | | | - Franck Lefèvre
- Laboratoire Atmospheres, Milieux, Observations Spatiales (LATMOS), IPSL, Paris, France
| | - Charles Miller
- NASA Jet Propulsion Laboratory, California Institute of Technology, Pasadena, California
| | - Michael Mischna
- NASA Jet Propulsion Laboratory, California Institute of Technology, Pasadena, California
| | - Michael Mumma
- NASA Goddard Space Flight Center, Greenbelt, Maryland
| | - Sally Newman
- California Institute of Technology, Pasadena, California
| | | | | | | | | | - Radu Popa
- University of Southern California, Los Angeles, California
| | - Michael Russell
- NASA Jet Propulsion Laboratory, California Institute of Technology, Pasadena, California
| | - Linhan Shen
- California Institute of Technology, Pasadena, California
| | | | - Robert Staehle
- NASA Jet Propulsion Laboratory, California Institute of Technology, Pasadena, California
| | - Vlada Stamenković
- California Institute of Technology, Pasadena, California
- NASA Jet Propulsion Laboratory, California Institute of Technology, Pasadena, California
| | | | | | - Ann C. Vandaele
- The Royal Belgian Institute for Space Aeronomy (BIRA-IASB), Brussels, Belgium
| | - Sébastien Viscardy
- The Royal Belgian Institute for Space Aeronomy (BIRA-IASB), Brussels, Belgium
| | - Christopher R. Webster
- NASA Jet Propulsion Laboratory, California Institute of Technology, Pasadena, California
| | | | | | - John Worden
- NASA Jet Propulsion Laboratory, California Institute of Technology, Pasadena, California
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17
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Guzewich SD, Newman CE, Smith MD, Moores JE, Smith CL, Moore C, Richardson MI, Kass D, Kleinböhl A, Mischna M, Martín-Torres FJ, Zorzano-Mier MP, Battalio M. The Vertical Dust Profile over Gale Crater, Mars. JOURNAL OF GEOPHYSICAL RESEARCH. PLANETS 2017; 122:2779-2792. [PMID: 32523861 PMCID: PMC7285022 DOI: 10.1002/2017je005420] [Citation(s) in RCA: 1] [Impact Index Per Article: 0.1] [Reference Citation Analysis] [Abstract] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 06/10/2023]
Abstract
We create a vertically coarse, but complete, vertical profile of dust mixing ratio from the surface to the upper atmosphere over Gale Crater, Mars, using the frequent joint atmospheric observations of the orbiting Mars Climate Sounder (MCS) and the Mars Science Laboratory (MSL) Curiosity rover. Using these data and an estimate of planetary boundary layer (PBL) depth from the MarsWRF general circulation model, we divide the vertical column into three regions. The first region is the Gale Crater PBL, the second is the MCS-sampled region, and the third is between these first two. We solve for a well-mixed dust mixing ratio within this third (middle) layer of atmosphere to complete the profile. We identify a unique seasonal cycle of dust within each atmospheric layer. Within the Gale PBL, dust mixing ratio maximizes near southern hemisphere summer solstice (Ls = 270°) and minimizes near winter solstice (Ls = 90-100°) with a smooth sinusoidal transition between them. However, the layer above Gale Crater and below the MCS-sampled region more closely follows the global opacity cycle and has a maximum in opacity near Ls = 240° and exhibits a local minimum (associated with the "solsticial pause" in dust storm activity) near Ls = 270°. With knowledge of the complete vertical dust profile, we can also assess the frequency of high-altitude dust layers over Gale. We determine that 36% of MCS profiles near Gale Crater contain an "absolute" high-altitude dust layer wherein the dust mixing ratio is the maximum in the entire vertical column.
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Affiliation(s)
- Scott D Guzewich
- NASA Goddard Spaceflight Center, 8800 Greenbelt Road, Code 693, Greenbelt, MD 20771
| | | | - M D Smith
- NASA Goddard Spaceflight Center, 8800 Greenbelt Road, Code 693, Greenbelt, MD 20771
| | - J E Moores
- York University, Department of Earth and Space Science and Engineering, Toronto, ON, Canada M3J 1P3
| | - C L Smith
- York University, Department of Earth and Space Science and Engineering, Toronto, ON, Canada M3J 1P3
| | - C Moore
- York University, Department of Earth and Space Science and Engineering, Toronto, ON, Canada M3J 1P3
| | | | - D Kass
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109
| | - A Kleinböhl
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109
| | - M Mischna
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109
| | - F J Martín-Torres
- Division of Space Technology, Department of Computer Science, Electrical and Space Engineering, Luleå University of Technology, Kiruna, Sweden; Instituto Andaluz de Ciencias de la Tierra (CSIC-UGR), 18100 Granada, Spain
| | - M-P Zorzano-Mier
- Division of Space Technology, Department of Computer Science, Electrical and Space Engineering, Luleå University of Technology, Kiruna, Sweden; Centro de Astrobiología (INTA-CSIC), Torrejón de Ardoz, 28850 Madrid, Spain
| | - M Battalio
- Texas A&M University, Department of Atmospheric Sciences, College Station, TX 77843
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Resolving Orbital and Climate Keys of Earth and Extraterrestrial Environments with Dynamics (ROCKE-3D) 1.0: A General Circulation Model for Simulating the Climates of Rocky Planets. ACTA ACUST UNITED AC 2017. [DOI: 10.3847/1538-4365/aa7a06] [Citation(s) in RCA: 84] [Impact Index Per Article: 12.0] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/18/2022]
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19
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Newman CE, Gómez-Elvira J, Marin M, Navarro S, Torres J, Richardson MI, Battalio JM, Guzewich SD, Sullivan R, de la Torre M, Vasavada AR, Bridges NT. Winds measured by the Rover Environmental Monitoring Station (REMS) during the Mars Science Laboratory (MSL) rover's Bagnold Dunes Campaign and comparison with numerical modeling using MarsWRF. ICARUS 2017; 291:203-231. [PMID: 30393391 PMCID: PMC6208171 DOI: 10.1016/j.icarus.2016.12.016] [Citation(s) in RCA: 6] [Impact Index Per Article: 0.9] [Reference Citation Analysis] [Abstract] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 05/16/2023]
Abstract
A high density of REMS wind measurements were collected in three science investigations during MSL's Bagnold Dunes Campaign, which took place over ~80 sols around southern winter solstice (Ls~90°) and constituted the first in situ analysis of the environmental conditions, morphology, structure, and composition of an active dune field on Mars. The Wind Characterization Investigation was designed to Available online 14 December 2016 fully characterize the near-surface wind field just outside the dunes and confirmed the primarily upslope/downslope flow expected from theory and modeling of the circulation on the slopes of Aeolis Mons in this season. The basic pattern of winds is 'upslope' (from the northwest, heading up Aeolis Mons) during the daytime (~09:00-17:00 or 18:00) and 'downslope' (from the southeast, heading down Aeolis Mons) at night (~20:00 to some time before 08:00). Between these times the wind rotates largely clockwise, giving generally westerly winds mid-morning and easterly winds in the early evening. The timings of these direction changes are relatively consistent from sol to sol; however, the wind direction and speed at any given time shows considerable intersol variability. This pattern and timing is similar to predictions from the MarsWRF numerical model, run at a resolution of ~490 m in this region, although the model predicts the upslope winds to have a stronger component from the E than the W, misses a wind speed peak at ~09:00, and under-predicts the strength of daytime wind speeds by ~2-4 m/s. The Namib Dune Lee Investigation reveals 'blocking' of northerly winds by the dune, leaving primarily a westerly component to the daytime winds, and also shows a broadening of the 1 Hz wind speed distribution likely associated with lee turbulence. The Namib Dune Side Investigation measured primarily daytime winds at the side of the same dune, in support of aeolian change detection experiments designed to put limits on the saltation threshold, and also appears to show the influence of the dune body on the local flow, though less clearly than in the lee. Using a vertical grid with lower resolution near the surface reduces the relative strength of nighttime winds predicted by MarsWRF and produces a peak in wind speed at ~09:00, improving the match to the observed diurnal variation of wind speed, albeit with an offset in magnitude. The annual wind field predicted using this grid also provides a far better match to observations of aeolian dune morphology and motion in the Bagnold Dunes. However, the lower overall wind speeds than observed and disagreement with the observed wind direction at ~09:00 suggest that the problem has not been solved and that alternative boundary layer mixing schemes should be explored which may result in more mixing of momentum down to the near-surface from higher layers. These results demonstrate a strong need for in situ wind data to constrain the setup and assumptions used in numerical models, so that they may be used with more confidence to predict the circulation at other times and locations on Mars.
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Affiliation(s)
- Claire E. Newman
- Aeolis Research, Pasadena, CA 91107, USA
- Corresponding author: (C.E. Newman)
| | | | - Mercedes Marin
- Centro de AAstrobiología (CSIC-INTA), Torrejón de Ardoz, Madrid, Spain
| | - Sara Navarro
- Centro de AAstrobiología (CSIC-INTA), Torrejón de Ardoz, Madrid, Spain
| | - Josefina Torres
- Centro de AAstrobiología (CSIC-INTA), Torrejón de Ardoz, Madrid, Spain
| | | | | | | | | | - Manuel de la Torre
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109, USA
| | - Ashwin R. Vasavada
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109, USA
| | - Nathan T. Bridges
- Johns Hopkins University Applied Physics Laboratory, Laurel, MD 20723, USA
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Diniega S, Hansen CJ, Allen A, Grigsby N, Li Z, Perez T, Chojnacki M. Dune-slope activity due to frost and wind throughout the north polar erg, Mars. GEOLOGICAL SOCIETY SPECIAL PUBLICATION 2017; 467. [PMID: 29731538 DOI: 10.1144/sp467.6] [Citation(s) in RCA: 13] [Impact Index Per Article: 1.9] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 11/04/2022]
Abstract
Repeat, high-resolution imaging of dunes within the Martian north polar erg have shown that these dune slopes are very active, with alcoves forming along the dune brink each Mars year. In some areas, a few hundred cubic metres of downslope sand movement have been observed, sometimes moving the dune brink 'backwards'. Based on morphological and activity-timing similarities of these north polar features to southern dune gullies, identifying the processes forming these features is likely to have relevance for understanding the general evolution/modification of dune gullies. To determine alcove-formation model constraints, we have surveyed seven dune fields, each over 1-4 Mars winters. Consistent with earlier reports, we found that alcove-formation activity occurs during the autumn-winter seasons, before or while the stable seasonal frost layer is deposited. We propose a new model in which alcove formation occurs during the autumn, and springtime sublimation activity then enhances the feature. Summertime winds blow sand into the new alcoves, erasing small alcoves over a few Mars years. Based on the observed rate of alcove erasure, we estimated the effective aeolian sand transport flux. From this, we proposed that alcove formation may account for 2-20% of the total sand movement within these dune fields.
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Affiliation(s)
- Serina Diniega
- Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, M/S 321-630, Pasadena, CA 91109 USA
| | - Candice J Hansen
- Planetary Science Institute, 1700 E. Fort Lowell, Tucson, AZ 85719, USA
| | - Amanda Allen
- Santa Barbara City College, 721 Cliff Drive, Santa Barbara, CA 93109, USA
| | - Nathan Grigsby
- Boise State University, 1910 University Drive, Boise, ID 83725, USA
| | - Zheyu Li
- University of Oxford, Oxford OX1 2JD, UK
| | - Tyler Perez
- California Institute of Technology, Pasadena, CA 91125, USA
| | - Matthew Chojnacki
- Lunar and Planetary Laboratory, University of Arizona, 1629 E University Blvd, Tucson, AZ 85721, USA
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Harri AM, Genzer M, Kemppinen O, Gomez-Elvira J, Haberle R, Polkko J, Savijärvi H, Rennó N, Rodriguez-Manfredi JA, Schmidt W, Richardson M, Siili T, Paton M, Torre-Juarez MDL, Mäkinen T, Newman C, Rafkin S, Mischna M, Merikallio S, Haukka H, Martin-Torres J, Komu M, Zorzano MP, Peinado V, Vazquez L, Urqui R. Mars Science Laboratory relative humidity observations: Initial results. JOURNAL OF GEOPHYSICAL RESEARCH. PLANETS 2014; 119:2132-2147. [PMID: 26213667 PMCID: PMC4508910 DOI: 10.1002/2013je004514] [Citation(s) in RCA: 6] [Impact Index Per Article: 0.6] [Reference Citation Analysis] [Abstract] [Key Words] [Track Full Text] [Subscribe] [Scholar Register] [Received: 09/01/2013] [Accepted: 07/08/2014] [Indexed: 05/28/2023]
Abstract
UNLABELLED The Mars Science Laboratory (MSL) made a successful landing at Gale crater early August 2012. MSL has an environmental instrument package called the Rover Environmental Monitoring Station (REMS) as a part of its scientific payload. REMS comprises instrumentation for the observation of atmospheric pressure, temperature of the air, ground temperature, wind speed and direction, relative humidity (REMS-H), and UV measurements. We concentrate on describing the REMS-H measurement performance and initial observations during the first 100 MSL sols as well as constraining the REMS-H results by comparing them with earlier observations and modeling results. The REMS-H device is based on polymeric capacitive humidity sensors developed by Vaisala Inc., and it makes use of transducer electronics section placed in the vicinity of the three humidity sensor heads. The humidity device is mounted on the REMS boom providing ventilation with the ambient atmosphere through a filter protecting the device from airborne dust. The final relative humidity results appear to be convincing and are aligned with earlier indirect observations of the total atmospheric precipitable water content. The water mixing ratio in the atmospheric surface layer appears to vary between 30 and 75 ppm. When assuming uniform mixing, the precipitable water content of the atmosphere is ranging from a few to six precipitable micrometers. KEY POINTS Atmospheric water mixing ratio at Gale crater varies from 30 to 140 ppmMSL relative humidity observation provides good dataHighest detected relative humidity reading during first MSL 100 sols is RH75.
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Affiliation(s)
- A-M Harri
- Finnish Meteorological Institute Helsinki, Finland
| | - M Genzer
- Finnish Meteorological Institute Helsinki, Finland
| | - O Kemppinen
- Finnish Meteorological Institute Helsinki, Finland
| | | | - R Haberle
- NASA AMES Research Center San Francisco, California, USA
| | - J Polkko
- Finnish Meteorological Institute Helsinki, Finland
| | - H Savijärvi
- Finnish Meteorological Institute Helsinki, Finland
| | - N Rennó
- Department of Atmospheric, Oceanic and Space Sciences, University of Michigan Ann Arbor, Michigan, USA
| | | | - W Schmidt
- Finnish Meteorological Institute Helsinki, Finland
| | | | - T Siili
- Finnish Meteorological Institute Helsinki, Finland
| | - M Paton
- Finnish Meteorological Institute Helsinki, Finland
| | | | - T Mäkinen
- Finnish Meteorological Institute Helsinki, Finland
| | - C Newman
- Ashima Research Inc. Pasadena, California, USA
| | - S Rafkin
- Southwest Research Institute Boulder, Colorado, USA
| | - M Mischna
- NASA Jet Propulsion Laboratory Pasadena, California, USA
| | - S Merikallio
- Finnish Meteorological Institute Helsinki, Finland
| | - H Haukka
- Finnish Meteorological Institute Helsinki, Finland
| | | | - M Komu
- Finnish Meteorological Institute Helsinki, Finland
| | | | - V Peinado
- Centro de Astrobiologia Madrid, Spain
| | - L Vazquez
- Department of Applied Mathematics, Complutense University of Madrid Madrid, Spain
| | - R Urqui
- Centro de Astrobiologia Madrid, Spain
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22
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Harri AM, Genzer M, Kemppinen O, Gomez-Elvira J, Haberle R, Polkko J, Savijärvi H, Rennó N, Rodriguez-Manfredi JA, Schmidt W, Richardson M, Siili T, Paton M, Torre-Juarez MDL, Mäkinen T, Newman C, Rafkin S, Mischna M, Merikallio S, Haukka H, Martin-Torres J, Komu M, Zorzano MP, Peinado V, Vazquez L, Urqui R. Mars Science Laboratory relative humidity observations: Initial results. JOURNAL OF GEOPHYSICAL RESEARCH. PLANETS 2014; 119:2132-2147. [PMID: 26213667 DOI: 10.1002/2013je004423] [Citation(s) in RCA: 7] [Impact Index Per Article: 0.7] [Reference Citation Analysis] [Abstract] [Key Words] [Track Full Text] [Subscribe] [Scholar Register] [Received: 09/01/2013] [Accepted: 07/08/2014] [Indexed: 05/28/2023]
Abstract
UNLABELLED The Mars Science Laboratory (MSL) made a successful landing at Gale crater early August 2012. MSL has an environmental instrument package called the Rover Environmental Monitoring Station (REMS) as a part of its scientific payload. REMS comprises instrumentation for the observation of atmospheric pressure, temperature of the air, ground temperature, wind speed and direction, relative humidity (REMS-H), and UV measurements. We concentrate on describing the REMS-H measurement performance and initial observations during the first 100 MSL sols as well as constraining the REMS-H results by comparing them with earlier observations and modeling results. The REMS-H device is based on polymeric capacitive humidity sensors developed by Vaisala Inc., and it makes use of transducer electronics section placed in the vicinity of the three humidity sensor heads. The humidity device is mounted on the REMS boom providing ventilation with the ambient atmosphere through a filter protecting the device from airborne dust. The final relative humidity results appear to be convincing and are aligned with earlier indirect observations of the total atmospheric precipitable water content. The water mixing ratio in the atmospheric surface layer appears to vary between 30 and 75 ppm. When assuming uniform mixing, the precipitable water content of the atmosphere is ranging from a few to six precipitable micrometers. KEY POINTS Atmospheric water mixing ratio at Gale crater varies from 30 to 140 ppmMSL relative humidity observation provides good dataHighest detected relative humidity reading during first MSL 100 sols is RH75.
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Affiliation(s)
- A-M Harri
- Finnish Meteorological Institute Helsinki, Finland
| | - M Genzer
- Finnish Meteorological Institute Helsinki, Finland
| | - O Kemppinen
- Finnish Meteorological Institute Helsinki, Finland
| | | | - R Haberle
- NASA AMES Research Center San Francisco, California, USA
| | - J Polkko
- Finnish Meteorological Institute Helsinki, Finland
| | - H Savijärvi
- Finnish Meteorological Institute Helsinki, Finland
| | - N Rennó
- Department of Atmospheric, Oceanic and Space Sciences, University of Michigan Ann Arbor, Michigan, USA
| | | | - W Schmidt
- Finnish Meteorological Institute Helsinki, Finland
| | | | - T Siili
- Finnish Meteorological Institute Helsinki, Finland
| | - M Paton
- Finnish Meteorological Institute Helsinki, Finland
| | | | - T Mäkinen
- Finnish Meteorological Institute Helsinki, Finland
| | - C Newman
- Ashima Research Inc. Pasadena, California, USA
| | - S Rafkin
- Southwest Research Institute Boulder, Colorado, USA
| | - M Mischna
- NASA Jet Propulsion Laboratory Pasadena, California, USA
| | - S Merikallio
- Finnish Meteorological Institute Helsinki, Finland
| | - H Haukka
- Finnish Meteorological Institute Helsinki, Finland
| | | | - M Komu
- Finnish Meteorological Institute Helsinki, Finland
| | | | - V Peinado
- Centro de Astrobiologia Madrid, Spain
| | - L Vazquez
- Department of Applied Mathematics, Complutense University of Madrid Madrid, Spain
| | - R Urqui
- Centro de Astrobiologia Madrid, Spain
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23
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Lebonnois S, Covey C, Grossman A, Parish H, Schubert G, Walterscheid R, Lauritzen P, Jablonowski C. Angular momentum budget in General Circulation Models of superrotating atmospheres: A critical diagnostic. ACTA ACUST UNITED AC 2012. [DOI: 10.1029/2012je004223] [Citation(s) in RCA: 29] [Impact Index Per Article: 2.4] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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24
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Greybush SJ, Wilson RJ, Hoffman RN, Hoffman MJ, Miyoshi T, Ide K, McConnochie T, Kalnay E. Ensemble Kalman filter data assimilation of Thermal Emission Spectrometer temperature retrievals into a Mars GCM. ACTA ACUST UNITED AC 2012. [DOI: 10.1029/2012je004097] [Citation(s) in RCA: 53] [Impact Index Per Article: 4.4] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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25
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Zhang Y, Karamchandani P, Glotfelty T, Streets DG, Grell G, Nenes A, Yu F, Bennartz R. Development and initial application of the global-through-urban weather research and forecasting model with chemistry (GU-WRF/Chem). ACTA ACUST UNITED AC 2012. [DOI: 10.1029/2012jd017966] [Citation(s) in RCA: 55] [Impact Index Per Article: 4.6] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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26
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Mischna MA, Lee C, Richardson M. Development of a fast, accurate radiative transfer model for the Martian atmosphere, past and present. ACTA ACUST UNITED AC 2012. [DOI: 10.1029/2012je004110] [Citation(s) in RCA: 40] [Impact Index Per Article: 3.3] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/10/2022]
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27
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Sprague AL, Boynton WV, Forget F, Lian Y, Richardson M, Starr R, Metzger AE, Hamara D, Economou T. Interannual similarity and variation in seasonal circulation of Mars' atmospheric Ar as seen by the Gamma Ray Spectrometer on Mars Odyssey. ACTA ACUST UNITED AC 2012. [DOI: 10.1029/2011je003873] [Citation(s) in RCA: 36] [Impact Index Per Article: 3.0] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/10/2022]
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28
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Guzewich SD, Talaat ER, Waugh DW. Observations of planetary waves and nonmigrating tides by the Mars Climate Sounder. ACTA ACUST UNITED AC 2012. [DOI: 10.1029/2011je003924] [Citation(s) in RCA: 34] [Impact Index Per Article: 2.8] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/10/2022]
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29
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Andrews-Hanna JC, Lewis KW. Early Mars hydrology: 2. Hydrological evolution in the Noachian and Hesperian epochs. ACTA ACUST UNITED AC 2011. [DOI: 10.1029/2010je003709] [Citation(s) in RCA: 94] [Impact Index Per Article: 7.2] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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30
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Eymet V, Fournier R, Dufresne JL, Lebonnois S, Hourdin F, Bullock MA. Net exchange parameterization of thermal infrared radiative transfer in Venus' atmosphere. ACTA ACUST UNITED AC 2009. [DOI: 10.1029/2008je003276] [Citation(s) in RCA: 41] [Impact Index Per Article: 2.7] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/10/2022]
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31
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Kleinböhl A, Schofield JT, Kass DM, Abdou WA, Backus CR, Sen B, Shirley JH, Lawson WG, Richardson MI, Taylor FW, Teanby NA, McCleese DJ. Mars Climate Sounder limb profile retrieval of atmospheric temperature, pressure, and dust and water ice opacity. ACTA ACUST UNITED AC 2009. [DOI: 10.1029/2009je003358] [Citation(s) in RCA: 182] [Impact Index Per Article: 12.1] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
Affiliation(s)
- Armin Kleinböhl
- Jet Propulsion Laboratory; California Institute of Technology; Pasadena California USA
| | - John T. Schofield
- Jet Propulsion Laboratory; California Institute of Technology; Pasadena California USA
| | - David M. Kass
- Jet Propulsion Laboratory; California Institute of Technology; Pasadena California USA
| | - Wedad A. Abdou
- Jet Propulsion Laboratory; California Institute of Technology; Pasadena California USA
| | - Charles R. Backus
- Jet Propulsion Laboratory; California Institute of Technology; Pasadena California USA
| | - Bhaswar Sen
- Jet Propulsion Laboratory; California Institute of Technology; Pasadena California USA
| | - James H. Shirley
- Jet Propulsion Laboratory; California Institute of Technology; Pasadena California USA
| | - W. Gregory Lawson
- Division of Geological and Planetary Sciences; California Institute of Technology; Pasadena California USA
| | - Mark I. Richardson
- Division of Geological and Planetary Sciences; California Institute of Technology; Pasadena California USA
| | - Fredric W. Taylor
- Clarendon Laboratory, Atmospheric, Oceanic, and Planetary Physics; University of Oxford; Oxford UK
| | - Nicholas A. Teanby
- Clarendon Laboratory, Atmospheric, Oceanic, and Planetary Physics; University of Oxford; Oxford UK
| | - Daniel J. McCleese
- Jet Propulsion Laboratory; California Institute of Technology; Pasadena California USA
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32
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Lee C, Lawson WG, Richardson MI, Heavens NG, Kleinböhl A, Banfield D, McCleese DJ, Zurek R, Kass D, Schofield JT, Leovy CB, Taylor FW, Toigo AD. Thermal Tides in the Martian Middle Atmosphere as Seen by the Mars Climate Sounder. JOURNAL OF GEOPHYSICAL RESEARCH 2009. [PMID: 27630378 DOI: 10.1029/2008je003302] [Citation(s) in RCA: 2] [Impact Index Per Article: 0.1] [Reference Citation Analysis] [Abstract] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 05/16/2023]
Abstract
The first systematic observations of the middle atmosphere of Mars (35km-80km) with the Mars Climate Sounder (MCS) show dramatic patterns of diurnal thermal variation, evident in retrievals of temperature and water ice opacity. At the time of writing, the dataset of MCS limb retrievals is sufficient for spectral analysis within a limited range of latitudes and seasons. This analysis shows that these thermal variations are almost exclusively associated with a diurnal thermal tide. Using a Martian General Circulation Model to extend our analysis we show that the diurnal thermal tide dominates these patterns for all latitudes and all seasons.
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Affiliation(s)
- C Lee
- Division of Geological and Planetary Sciences, California Institute of Technology
| | - W G Lawson
- Division of Geological and Planetary Sciences, California Institute of Technology
| | - M I Richardson
- Division of Geological and Planetary Sciences, California Institute of Technology
| | - N G Heavens
- Division of Geological and Planetary Sciences, California Institute of Technology
| | - A Kleinböhl
- Jet Propulsion Laboratory, California Institute of Technology
| | - D Banfield
- Department of Astronomy, Cornell University
| | - D J McCleese
- Jet Propulsion Laboratory, California Institute of Technology
| | - R Zurek
- Jet Propulsion Laboratory, California Institute of Technology
| | - D Kass
- Jet Propulsion Laboratory, California Institute of Technology
| | - J T Schofield
- Jet Propulsion Laboratory, California Institute of Technology
| | - C B Leovy
- Department of Atmospheric Sciences, University of Washington
| | - F W Taylor
- Department of Physics, University of Oxford
| | - A D Toigo
- Department of Astronomy, Cornell University
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33
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Lee C, Lawson WG, Richardson MI, Heavens NG, Kleinböhl A, Banfield D, McCleese DJ, Zurek R, Kass D, Schofield JT, Leovy CB, Taylor FW, Toigo AD. Thermal Tides in the Martian Middle Atmosphere as Seen by the Mars Climate Sounder. ACTA ACUST UNITED AC 2009; 114. [PMID: 27630378 DOI: 10.1029/2008je003285] [Citation(s) in RCA: 75] [Impact Index Per Article: 5.0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
Abstract
The first systematic observations of the middle atmosphere of Mars (35km-80km) with the Mars Climate Sounder (MCS) show dramatic patterns of diurnal thermal variation, evident in retrievals of temperature and water ice opacity. At the time of writing, the dataset of MCS limb retrievals is sufficient for spectral analysis within a limited range of latitudes and seasons. This analysis shows that these thermal variations are almost exclusively associated with a diurnal thermal tide. Using a Martian General Circulation Model to extend our analysis we show that the diurnal thermal tide dominates these patterns for all latitudes and all seasons.
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Affiliation(s)
- C Lee
- Division of Geological and Planetary Sciences, California Institute of Technology
| | - W G Lawson
- Division of Geological and Planetary Sciences, California Institute of Technology
| | - M I Richardson
- Division of Geological and Planetary Sciences, California Institute of Technology
| | - N G Heavens
- Division of Geological and Planetary Sciences, California Institute of Technology
| | - A Kleinböhl
- Jet Propulsion Laboratory, California Institute of Technology
| | - D Banfield
- Department of Astronomy, Cornell University
| | - D J McCleese
- Jet Propulsion Laboratory, California Institute of Technology
| | - R Zurek
- Jet Propulsion Laboratory, California Institute of Technology
| | - D Kass
- Jet Propulsion Laboratory, California Institute of Technology
| | - J T Schofield
- Jet Propulsion Laboratory, California Institute of Technology
| | - C B Leovy
- Department of Atmospheric Sciences, University of Washington
| | - F W Taylor
- Department of Physics, University of Oxford
| | - A D Toigo
- Department of Astronomy, Cornell University
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34
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Tokano T. The dynamics of Titan's troposphere. PHILOSOPHICAL TRANSACTIONS. SERIES A, MATHEMATICAL, PHYSICAL, AND ENGINEERING SCIENCES 2009; 367:633-648. [PMID: 19019782 DOI: 10.1098/rsta.2008.0163] [Citation(s) in RCA: 1] [Impact Index Per Article: 0.1] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 05/27/2023]
Abstract
While the Voyager mission could essentially not reveal the dynamics of Titan's troposphere, useful information was obtained by the Cassini spacecraft and, particularly, by the Huygens probe that landed on Titan's surface; this information can be interpreted by means of numerical models of atmospheric circulation. The meridional circulation is likely to consist of a large Hadley circulation asymmetric about the equator, but is susceptible to disruption by turbulence in clouds. The zonal wind in the troposphere is comparable to or even weaker than that in the terrestrial troposphere and contains zones of easterlies, much in contrast to the super-rotating stratosphere. Unique to Titan is the transition from a geostrophic to cyclostrophic wind balance in the upper troposphere. While Earth-like storm systems associated with baroclinic instability are absent, Saturn's gravitational tide introduces a planetary wave of wavenumber 2 and a periodical variation in the wind direction in the troposphere. Unlike on Earth, the wind over the equatorial surface is westerly. The seasonal reversal in the Hadley circulation sense and zonal wind direction is predicted to have a substantial influence on the formation of dunes as well as variation of Titan's rotation rate and length of day.
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Affiliation(s)
- Tetsuya Tokano
- Institut für Geophysik und Meteorologie, Universität zu Köln, Albertus-Magnus-Platz, 50923 Köln, Germany.
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35
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Teanby NA, Irwin PGJ, de Kok R, Nixon CA. Dynamical implications of seasonal and spatial variations in Titan's stratospheric composition. PHILOSOPHICAL TRANSACTIONS. SERIES A, MATHEMATICAL, PHYSICAL, AND ENGINEERING SCIENCES 2009; 367:697-711. [PMID: 19019781 DOI: 10.1098/rsta.2008.0164] [Citation(s) in RCA: 6] [Impact Index Per Article: 0.4] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 05/27/2023]
Abstract
Titan's diverse inventory of photochemically produced gases can be used as tracers to probe atmospheric circulation. Since the arrival of the Cassini-Huygens mission in July 2004 it has been possible to map the seasonal and spatial variations of these compounds in great detail. Here, we use 3.5 years of data measured by the Cassini Composite InfraRed Spectrometer instrument to determine spatial and seasonal composition trends, thus providing clues to underlying atmospheric motions. Titan's North Pole (currently in winter) displays enrichment of trace species, implying subsidence is occurring there. This is consistent with the descending branch of a single south-to-north stratospheric circulation cell and a polar vortex. Lack of enrichment in the south over most of the observed time period argues against the presence of any secondary circulation cell in the Southern Polar stratosphere. However, a residual cap of enriched gas was observed over the South Pole early in the mission, which has since completely dissipated. This cap was most probably due to residual build-up from southern winter. These observations provide new and important constraints for models of atmospheric photochemistry and circulation.
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Affiliation(s)
- Nicholas A Teanby
- Atmospheric, Oceanic & Planetary Physics, Clarendon Laboratory, Department of Physics, University of Oxford, Parks Road, Oxford OX1 3PU, UK.
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36
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Flasar FM, Achterberg RK. The structure and dynamics of Titan's middle atmosphere. PHILOSOPHICAL TRANSACTIONS. SERIES A, MATHEMATICAL, PHYSICAL, AND ENGINEERING SCIENCES 2009; 367:649-664. [PMID: 19073460 DOI: 10.1098/rsta.2008.0242] [Citation(s) in RCA: 3] [Impact Index Per Article: 0.2] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 05/27/2023]
Abstract
Titan's middle atmosphere is characterized by cyclostrophic winds and strong seasonal modulation. Cassini CIRS observations, obtained in northern winter, indicate that the stratosphere near 1mbar is warmest at low latitudes, with the South Pole a few degrees colder and the North Pole approximately 20K colder. Associated with the cold northern temperatures are strong circumpolar winds with speeds as high as 190ms-1. Within this vortex, the mixing ratios of several organic gases are enhanced relative to those at low latitudes. Comparison with Voyager thermal infrared measurements, obtained 25 years ago in northern spring, suggests that the enhancement currently observed will increase as the winter progresses. The stratopause height increases from 0.1mbar near the equator to 0.01mbar near the North Pole, where it is the warmest part of the atmosphere, greater than 200K. This implies subsidence at the pole, which is consistent with the enhanced organics observed. Condensate features, several still not identified, are also apparent in the infrared spectra at high northern latitudes. In many ways, the winter vortex observed on Titan, with cyclostrophic winds, resembles the polar winter vortices on the Earth, where the mean winds are geostrophic.
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Affiliation(s)
- F M Flasar
- NASA Goddard Space Flight Center, Code 693, Greenbelt, MD 20771, USA.
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37
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Spiga A, Forget F. A new model to simulate the Martian mesoscale and microscale atmospheric circulation: Validation and first results. ACTA ACUST UNITED AC 2009. [DOI: 10.1029/2008je003242] [Citation(s) in RCA: 98] [Impact Index Per Article: 6.5] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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38
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Teanby NA, de Kok R, Irwin PGJ, Osprey S, Vinatier S, Gierasch PJ, Read PL, Flasar FM, Conrath BJ, Achterberg RK, Bézard B, Nixon CA, Calcutt SB. Titan's winter polar vortex structure revealed by chemical tracers. ACTA ACUST UNITED AC 2008. [DOI: 10.1029/2008je003218] [Citation(s) in RCA: 52] [Impact Index Per Article: 3.3] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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39
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Johnson SS, Mischna MA, Grove TL, Zuber MT. Sulfur-induced greenhouse warming on early Mars. ACTA ACUST UNITED AC 2008. [DOI: 10.1029/2007je002962] [Citation(s) in RCA: 76] [Impact Index Per Article: 4.8] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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40
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Heavens NG, Richardson MI, Toigo AD. Two aerodynamic roughness maps derived from Mars Orbiter Laser Altimeter (MOLA) data and their effects on boundary layer properties in a Mars general circulation model (GCM). ACTA ACUST UNITED AC 2008. [DOI: 10.1029/2007je002991] [Citation(s) in RCA: 10] [Impact Index Per Article: 0.6] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/10/2022]
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