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Spatial Autocorrelation of Martian Surface Temperature and Its Spatio-Temporal Relationships with Near-Surface Environmental Factors across China’s Tianwen-1 Landing Zone. REMOTE SENSING 2021. [DOI: 10.3390/rs13112206] [Citation(s) in RCA: 3] [Impact Index Per Article: 1.0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 11/16/2022]
Abstract
Variations in the Martian surface temperature indicate patterns of surface energy exchange. The Martian surface temperature at a location is similar to those in adjacent locations; but, an understanding of temperature clusters in multiple locations will deepen our knowledge of planetary surface processes overall. The spatial coherence of the Martian surface temperature (ST) at different locations, the spatio-temporal variations in temperature clusters, and the relationships between ST and near-surface environmental factors, however, are not well understood. To fill this gap, we studied an area to the south of Utopia Planitia, the landing zone for the Tianwen-1 Mars Exploration mission. The spatial aggregation of three Martian ST indicators (STIs), including sol average temperature (SAT), sol temperature range (STR), and sol-to-sol temperature change (STC), were quantitatively evaluated using clustering analysis at the global and local scale. In addition, we also detected the spatio-temporal variations in relations between the STIs and seven potential driving factors, including thermal inertia, albedo, dust, elevation, slope, and zonal and meridional winds, across the study area during 81 to 111 sols in Martian years 29–32, based on a geographically and temporally weighted regression model (GTWR). We found that the SAT, STR, and STC were not randomly distributed over space but exhibited signs of significant spatial aggregation. Thermal inertia and dust made the greatest contribution to the fluctuation in STIs over time. The local surface temperature was likely affected by the slope, wind, and local circulation, especially in the area with a large slope and low thermal inertia. In addition, the sheltering effects of the mountains at the edge of the basin likely contributed to the spatial difference in SAT and STR. These results are a reminder that the spatio-temporal variation in the local driving factors associated with Martian surface temperature cannot be neglected. Our research contributes to the understanding of the surface environment that might compromise the survival and operations of the Tianwen-1 lander on the Martian surface.
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Briggs G, Klaasen K, Thorpe T, Wellman J, Baum W. Martian dynamical phenomena during June-November 1976: Viking Orbiter imaging results. ACTA ACUST UNITED AC 2012. [DOI: 10.1029/js082i028p04121] [Citation(s) in RCA: 87] [Impact Index Per Article: 7.3] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/10/2022]
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Farmer CB, Davies DW, Holland AL, Laporte DD, Doms PE. Mars: Water vapor observations from the Viking orbiters. ACTA ACUST UNITED AC 2012. [DOI: 10.1029/js082i028p04225] [Citation(s) in RCA: 164] [Impact Index Per Article: 13.7] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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Kieffer HH, Martin TZ, Peterfreund AR, Jakosky BM, Miner ED, Palluconi FD. Thermal and albedo mapping of Mars during the Viking primary mission. ACTA ACUST UNITED AC 2012. [DOI: 10.1029/js082i028p04249] [Citation(s) in RCA: 535] [Impact Index Per Article: 44.6] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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Masursky H, Boyce JM, Dial AL, Schaber GG, Strobell ME. Classification and time of formation of Martian channels based on Viking data. ACTA ACUST UNITED AC 2012. [DOI: 10.1029/js082i028p04016] [Citation(s) in RCA: 234] [Impact Index Per Article: 19.5] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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Davies DW, Farmer CB, Laporte DD. Behavior of volatiles in Mars' polar areas: A model incorporating new experimental data. ACTA ACUST UNITED AC 2012. [DOI: 10.1029/jb082i026p03815] [Citation(s) in RCA: 49] [Impact Index Per Article: 4.1] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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Hayne PO, Paige DA, Schofield JT, Kass DM, Kleinböhl A, Heavens NG, McCleese DJ. Carbon dioxide snow clouds on Mars: South polar winter observations by the Mars Climate Sounder. ACTA ACUST UNITED AC 2012. [DOI: 10.1029/2011je004040] [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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Cornwall C, Titus TN. Spatial and temporal distributions of Martian north polar cold spots before, during, and after the global dust storm of 2001. ACTA ACUST UNITED AC 2009. [DOI: 10.1029/2008je003243] [Citation(s) in RCA: 14] [Impact Index Per Article: 0.9] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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Sprague AL, Boynton WV, Kerry KE, Janes DM, Kelly NJ, Crombie MK, Nelli SM, Murphy JR, Reedy RC, Metzger AE. Mars' atmospheric argon: Tracer for understanding Martian atmospheric circulation and dynamics. ACTA ACUST UNITED AC 2007. [DOI: 10.1029/2005je002597] [Citation(s) in RCA: 49] [Impact Index Per Article: 2.9] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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10
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Wolff MJ, Smith MD, Clancy RT, Spanovich N, Whitney BA, Lemmon MT, Bandfield JL, Banfield D, Ghosh A, Landis G, Christensen PR, Bell JF, Squyres SW. Constraints on dust aerosols from the Mars Exploration Rovers using MGS overflights and Mini-TES. ACTA ACUST UNITED AC 2006. [DOI: 10.1029/2006je002786] [Citation(s) in RCA: 132] [Impact Index Per Article: 7.3] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
Affiliation(s)
- M. J. Wolff
- Space Science Institute; Boulder Colorado USA
| | - M. D. Smith
- Goddard Space Flight Center; Greenbelt Maryland USA
| | | | - N. Spanovich
- Jet Propulsion Laboratory; California Institute of Technology; Pasadena California USA
| | | | - M. T. Lemmon
- Department of Atmospheric Sciences; Texas A&M University; College Station Texas USA
| | - J. L. Bandfield
- Department of Geological Sciences; Arizona State University; Tempe Arizona USA
| | - D. Banfield
- Department of Astronomy; Cornell University; Ithaca New York USA
| | - A. Ghosh
- Department of Earth and Planetary Sciences; University of Tennessee; Knoxville Tennessee USA
| | - G. Landis
- Photovoltaics and Space Environment Branch; NASA John Glenn Research Center; Cleveland Ohio USA
| | - P. R. Christensen
- Department of Geological Sciences; Arizona State University; Tempe Arizona USA
| | - J. F. Bell
- Department of Astronomy; Cornell University; Ithaca New York USA
| | - S. W. Squyres
- Department of Astronomy; Cornell University; Ithaca New York USA
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Sprague AL, Boynton WV, Kerry KE, Janes DM, Hunten DM, Kim KJ, Reedy RC, Metzger AE. Mars' South Polar Ar Enhancement: A Tracer for South Polar Seasonal Meridional Mixing. Science 2004; 306:1364-7. [PMID: 15472041 DOI: 10.1126/science.1098496] [Citation(s) in RCA: 59] [Impact Index Per Article: 3.0] [Reference Citation Analysis] [Abstract] [MESH Headings] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/02/2022]
Abstract
The gamma ray spectrometer on the Mars Odyssey spacecraft measured an enhancement of atmospheric argon over southern high latitudes during autumn followed by dissipation during winter and spring. Argon does not freeze at temperatures normal for southern winter (approximately 145 kelvin) and is left in the atmosphere, enriched relative to carbon dioxide (CO2), as the southern seasonal cap of CO2 frost accumulates. Calculations of seasonal transport of argon into and out of southern high latitudes point to meridional (north-south) mixing throughout southern winter and spring.
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Affiliation(s)
- A L Sprague
- Lunar and Planetary Laboratory, 1629 East University Boulevard, University of Arizona, Tucson, AZ 85721-0092, USA.
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Ramsey MS. Ejecta distribution patterns at Meteor Crater, Arizona: On the applicability of lithologic end-member deconvolution for spaceborne thermal infrared data of Earth and Mars. ACTA ACUST UNITED AC 2002. [DOI: 10.1029/2001je001827] [Citation(s) in RCA: 21] [Impact Index Per Article: 1.0] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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Titus TN, Kieffer HH, Mullins KF, Christensen PR. TES premapping data: Slab ice and snow flurries in the Martian north polar night. ACTA ACUST UNITED AC 2001. [DOI: 10.1029/2000je001284] [Citation(s) in RCA: 50] [Impact Index Per Article: 2.2] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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17
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Christensen PR, Bandfield JL, Hamilton VE, Ruff SW, Kieffer HH, Titus TN, Malin MC, Morris RV, Lane MD, Clark RL, Jakosky BM, Mellon MT, Pearl JC, Conrath BJ, Smith MD, Clancy RT, Kuzmin RO, Roush T, Mehall GL, Gorelick N, Bender K, Murray K, Dason S, Greene E, Silverman S, Greenfield M. Mars Global Surveyor Thermal Emission Spectrometer experiment: Investigation description and surface science results. ACTA ACUST UNITED AC 2001. [DOI: 10.1029/2000je001370] [Citation(s) in RCA: 782] [Impact Index Per Article: 34.0] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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18
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Kieffer HH, Titus TN, Mullins KF, Christensen PR. Mars south polar spring and summer behavior observed by TES: Seasonal cap evolution controlled by frost grain size. ACTA ACUST UNITED AC 2000. [DOI: 10.1029/1999je001136] [Citation(s) in RCA: 179] [Impact Index Per Article: 7.5] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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19
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Clancy RT, Sandor BJ, Wolff MJ, Christensen PR, Smith MD, Pearl JC, Conrath BJ, Wilson RJ. An intercomparison of ground-based millimeter, MGS TES, and Viking atmospheric temperature measurements: Seasonal and interannual variability of temperatures and dust loading in the global Mars atmosphere. ACTA ACUST UNITED AC 2000. [DOI: 10.1029/1999je001089] [Citation(s) in RCA: 295] [Impact Index Per Article: 12.3] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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20
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Forget F, Hourdin F, Fournier R, Hourdin C, Talagrand O, Collins M, Lewis SR, Read PL, Huot JP. Improved general circulation models of the Martian atmosphere from the surface to above 80 km. ACTA ACUST UNITED AC 1999. [DOI: 10.1029/1999je001025] [Citation(s) in RCA: 816] [Impact Index Per Article: 32.6] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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21
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Hansen GB. Control of the radiative behavior of the Martian polar caps by surface CO2ice: Evidence from Mars Global Surveyor measurements. ACTA ACUST UNITED AC 1999. [DOI: 10.1029/1998je000626] [Citation(s) in RCA: 52] [Impact Index Per Article: 2.1] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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22
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Christensen PR, Anderson DL, Chase SC, Clancy RT, Clark RN, Conrath BJ, Kieffer HH, Kuzmin RO, Malin MC, Pearl JC, Roush TL, Smith MD. Results from the Mars Global Surveyor Thermal Emission Spectrometer. Science 1998; 279:1692-8. [PMID: 9497282 DOI: 10.1126/science.279.5357.1692] [Citation(s) in RCA: 175] [Impact Index Per Article: 6.7] [Reference Citation Analysis] [Abstract] [Key Words] [MESH Headings] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/02/2022]
Abstract
The Thermal Emission Spectrometer spectra of low albedo surface materials suggests that a four to one mixture of pyroxene to plagioclase, together with about a 35 percent dust component provides the best fit to the spectrum. Qualitative upper limits can be placed on the concentration of carbonates (<10 percent), olivine (<10 percent), clay minerals (<20 percent), and quartz (<5 percent) in the limited regions observed. Limb observations in the northern hemisphere reveal low-lying dust hazes and detached water-ice clouds at altitudes up to 55 kilometers. At an aerocentric longitude of 224 degrees a major dust storm developed in the Noachis Terra region. The south polar cap retreat was similar to that observed by Viking.
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23
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Mars CO2 Ice Polar Caps. ACTA ACUST UNITED AC 1998. [DOI: 10.1007/978-94-011-5252-5_20] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register]
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24
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Hansen GB. The infrared absorption spectrum of carbon dioxide ice from 1.8 to 333 μm. ACTA ACUST UNITED AC 1997. [DOI: 10.1029/97je01875] [Citation(s) in RCA: 86] [Impact Index Per Article: 3.2] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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25
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Forget F, Pollack JB. Thermal infrared observations of the condensing Martian polar caps: CO2ice temperatures and radiative budget. ACTA ACUST UNITED AC 1996. [DOI: 10.1029/96je01077] [Citation(s) in RCA: 39] [Impact Index Per Article: 1.4] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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26
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Forget F, Hansen GB, Pollack JB. Low brightness temperatures of Martian polar caps: CO2clouds or low surface emissivity? ACTA ACUST UNITED AC 1995. [DOI: 10.1029/95je02378] [Citation(s) in RCA: 50] [Impact Index Per Article: 1.7] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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27
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Warren SG, Wiscombe WJ, Firestone JF. Spectral albedo and emissivity of CO2in Martian polar caps: Model results. ACTA ACUST UNITED AC 1990. [DOI: 10.1029/jb095ib09p14717] [Citation(s) in RCA: 59] [Impact Index Per Article: 1.7] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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28
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Paige DA, Herkenhoff KE, Murray BC. Mariner 9 observations of the south polar cap of Mars: Evidence for residual CO2frost. ACTA ACUST UNITED AC 1990. [DOI: 10.1029/jb095ib02p01319] [Citation(s) in RCA: 35] [Impact Index Per Article: 1.0] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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Brown WL, Lanzerotti LJ, Johnson RE. Fast Ion Bombardment of Ices and Its Astrophysical Implications. Science 1982; 218:525-31. [PMID: 17842043 DOI: 10.1126/science.218.4572.525] [Citation(s) in RCA: 105] [Impact Index Per Article: 2.5] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/02/2022]
Abstract
Ices such as water, carbon dioxide, and methane are now known to be pervasive constituents of the solar system and probably of the interstellar medium as well. Many of these ices and ice-covered surfaces are exposed to bombardment by the energetic ions of space. Laboratory experiments have been carried out to study the effects of such bombardment. Surprisingly efficient erosion of ice layers is associated with electronic excitation of the ices by the ions. These results are a challenge to an understanding of the physical processes involved and have implications for a number of astrophysical problems of current interest.
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Martin TZ, Kieffer HH. Thermal infrared properties of the Martian atmosphere: 2. The 15-μm band measurements. ACTA ACUST UNITED AC 1979. [DOI: 10.1029/jb084ib06p02843] [Citation(s) in RCA: 105] [Impact Index Per Article: 2.3] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/10/2022]
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33
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Martin TZ, Peterfreund AR, Miner ED, Kieffer HH, Hunt GE. Thermal infrared properties of the Martian atmosphere: 1. Global behavior at 7, 9, 11, and 20 μm. ACTA ACUST UNITED AC 1979. [DOI: 10.1029/jb084ib06p02830] [Citation(s) in RCA: 70] [Impact Index Per Article: 1.6] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/10/2022]
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34
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Hess SL. Static stability and thermal wind in an atmosphere of variable composition: Applications to Mars. ACTA ACUST UNITED AC 1979. [DOI: 10.1029/jb084ib06p02969] [Citation(s) in RCA: 21] [Impact Index Per Article: 0.5] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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35
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Jakosky BM. The effects of nonideal surfaces on the derived thermal properties of Mars. ACTA ACUST UNITED AC 1979. [DOI: 10.1029/jb084ib14p08252] [Citation(s) in RCA: 61] [Impact Index Per Article: 1.4] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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36
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Seiff A, Kirk DB. Structure of Mars' Atmosphere up to 100 Kilometers from the Entry Measurements of Viking 2. Science 1976; 194:1300-3. [PMID: 17797089 DOI: 10.1126/science.194.4271.1300] [Citation(s) in RCA: 37] [Impact Index Per Article: 0.8] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/02/2022]
Abstract
The Viking 2 entry science data on the structure of Mars' atmosphere up to 100 kilometers define a morning atmosphere with an isothermal region near the surface; a surface pressure 10 percent greater than that recorded simultaneously at the Viking 1 site, which implies a landing site elevation lower by 2.7 kilometers than the reference ellipsoid; and a thermal structure to 100 kilometers at least qualitatively consistent with pre-Viking modeling of thermal tides. The temperature profile exhibits waves whose amplitude grows with altitude, to approximately 25 degrees K at 90 kilometers. These waves are believed to be a consequence of layered vertical oscillations and associated heating and cooling by compression and expansion, excited by the daily thermal cycling of the planet surface. As is necessary for gravity wave propagation, the atmosphere is stable against convection, except possibly in some very local regions. Temperature is everywhere appreciably above the carbon dioxide condensation boundary at both landing sites, precluding the occurrence of carbon dioxide hazes in northern summer at latitudes to at least 50 degrees N. Thus, ground level mists seen in these latitudes would appear to be condensed water vapor.
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37
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Abstract
The annual temperature range for the martian surface at the Viking lander sites is computed on the basis of thermal parameters derived from observations made with the infrared thermal mappers. The Viking lander 1 (VL1) site has small annual variations in temperature, whereas the Viking lander 2 (VL2) site has large annual changes. With the Viking lander images used to estimate the rock component of the thermal emission, the daily temperature behavior of the soil alone is computed over the range of depths accessible to the lander; when the VL1 and VL2 sites were sampled, the daily temperature ranges at the top of the soil were 183 to 263 K and 183 to 268 K, respectively. The diurnal variation decreases with depth with an exponential scale of about 5 centimeters. The maximum temperature of the soil sampled from beneath rocks at the VL2 site is calculated to be 230 K. These temperature calculations should provide a reference for study of the active chemistry reported for the martian soil.
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Hess SL, Henry RM, Leovy CB, Mitchell JL, Ryan JA, Tillman JE. Early Meteorological Results from the Viking 2 Lander. Science 1976; 194:1352-3. [PMID: 17797100 DOI: 10.1126/science.194.4271.1352] [Citation(s) in RCA: 27] [Impact Index Per Article: 0.6] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/02/2022]
Abstract
Early results from the meteorological instruments on the Viking 2 lander are presented. As on lander 1, the daily patterns of temperature, wind, and pressure have been highly repetitive during the early summer period. The average daily maximum temperature was 241 degrees K and the diurnal minimum was 191 degrees K. The wind has a vector mean of 0.7 meter per second from the southeast with a diurnal amplitude of 3 meters per second. Pressure exhibits both diurnal and semidiurnal oscillations, although of substantially smaller amplitude than those of lander 1. Departures from the repetitive diurnal patterns begin to appear on sol 37.
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Abstract
The two Viking missions to Mars have been extraordinarily successful. Thirteen scientific investigations yielded information about the atmosphere and surface. Two orbiters and landers operating for several months photographed the surface extensively from 1500 kilometers and directly on the surface. Measurements were made of the atmospheric composition, the surface elemental abundance, the atmospheric water vapor, temperature of the surface, and meteorological conditions; direct tests were made for organic material and living organisms. The question of life on Mars remains unanswered. The Viking spacecraft are designed to continue the investigations for at least one Mars year.
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Farmer CB, Davies DW, Laporte DD. Mars: Northern Summer Ice Cap—Water Vapor Observations from Viking 2. Science 1976; 194:1339-41. [PMID: 17797096 DOI: 10.1126/science.194.4271.1339] [Citation(s) in RCA: 103] [Impact Index Per Article: 2.1] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/02/2022]
Abstract
Observations of the latitude dependence of water vapor made from the Viking 2 orbiter show peak abundances in the latitude band 70 degrees to 80 degrees north in the northern midsummer season (planetocentric longitude approximately 108 degrees ). Total column abundances in the polar regions require near-surface atmospheric temperatures in excess of 200 degrees K, and are incompatible with the survival of a frozen carbon dioxide cap at martian pressures. The remnant (or residual) north polar cap, and the outlying patches of ice at lower latitudes, are thus predominantly water ice, whose thickness can be estimated to be between 1 meter and 1 kilometer.
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Kieffer HH, Chase SC, Martin TZ, Miner ED, Palluconi FD. Martian North Pole Summer Temperatures: Dirty Water Ice. Science 1976; 194:1341-4. [PMID: 17797097 DOI: 10.1126/science.194.4271.1341] [Citation(s) in RCA: 218] [Impact Index Per Article: 4.5] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/02/2022]
Abstract
Broadband thermal and reflectance observations of the martian north polar region in late summer yield temperatures for the residual polar cap near 205 K with albedos near 43 percent. The residual cap and several outlying smaller deposits are water ice with included dirt; there is no evidence for any permanent carbon dioxide polar cap.
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Kieffer HH, Christensen PR, Martin TZ, Miner ED, Palluconi FD. Temperatures of the Martian Surface and Atmosphere: Viking Observation of Diurnal and Geometric Variations. Science 1976; 194:1346-51. [PMID: 17797099 DOI: 10.1126/science.194.4271.1346] [Citation(s) in RCA: 42] [Impact Index Per Article: 0.9] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/02/2022]
Abstract
Selected observations made with the Viking infrared thermal mapper after the first landing are reported. Atmospheric temperatures measured at the latitude of the Viking 2 landing site (48 degrees N) over most of a martian day reveal a diurnal variation of at least 15 K, with peak temperatures occurring near 2.2 hours after noon, implying significant absorption of sunlight in the lower 30 km of the atmosphere by entrained dust. The summit temperature of Arsia Mons varies by a factor of nearly two each day; large diurnal temperature variation is characteristic of the south Tharsis upland and implies the presence of low thermal inertia material. The thermal inertia of material on the floors of several typical large craters is found to be higher than for the surrounding terrain; this suggests that craters are somehow effective in sorting aeolian material. Brightness temperatures of the Viking 1 landing area decrease at large emission angles; the intensity of reflected sunlight shows a more complex dependence on geometry than expected, implying atmospheric as well as surface scattering.
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Hess SL, Henry RM, Leovy CB, Ryan JA, Tillman JE, Chamberlain TE, Cole HL, Dutton RG, Greene GC, Simon WE, Mitchell JL. Preliminary Meteorological Results on Mars from the Viking 1 Lander. Science 1976; 193:788-91. [PMID: 17747781 DOI: 10.1126/science.193.4255.788] [Citation(s) in RCA: 52] [Impact Index Per Article: 1.1] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/02/2022]
Abstract
The results from the meteorology instruments on the Viking 1 lander are presented for the first 4 sols of operation. The instruments are working satisfactorily. Temperatures fluctuated from a low of 188 degrees K to an estimated maximum of 244 degrees K. The mean pressure is 7.65 millibars with a diurnal variation of amplitude 0.1 millibar. Wind speeds averaged over several minutes have ranged from essentially calm to 9 meters per second. Wind directions have exhibited a remarkable regularity which may be associated with nocturnal downslope winds and gravitational oscillations, or to tidal effects of the diurnal pressure wave, or to both.
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