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

Clancy, R. T.; Sandor, Brad J.; Wolff, Michael; Christensen, P. R.; Smith, M. D.; Pearl, J. C.; Conrath, B. J.; Wilson, R. J.

doi:10.1029/1999je001089

Cited by 364 publications

(240 citation statements)

References 53 publications

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“…Further study with MGCM simulations is underway to better understand how to compare disk-averaged observations to spatially (and temporally) resolved model and spacecraft data. The close correspondence between MGS TES and microwave temperatures at 0.3-mb (Clancy et al 2000) supports the utility of the microwave data, and the multi-year record of microwave observations provides further evidence that the aphelion season is one of little variability.…”

Section: Interannual Variability Of Aphelion Season Temperaturesmentioning

confidence: 61%

The Martian Atmosphere During the Viking Mission, I Infrared Measurements of Atmospheric Temperatures Revisited

Wilson¹

2000

Icarus

112

135

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The Viking Infrared Thermal Mapper 15-µm channel brightness temperature observations (IRTM T 15 ) provide extensive spatial and temporal coverage of martian atmospheric temperatures on diurnal to seasonal time scales. The 15-µm channel was designed so that these temperatures would be representative of a deep layer of atmosphere centered at 0.5 mb (∼25 km). Our re-examination of the IRTM data indicates that the 15-µm channel was additionally sensitive to surface radiance so that air temperature determinations (nominal T 15 ) are significantly biased when the thermal contrast between the surface and atmosphere is large. This bias is suggested by the strong correlation between the diurnal variation of tropical T 15 and surface temperatures for non-dust-storm conditions. We show that numerical modeling of the thermal tides provides a basis for distinguishing between the surface and atmospheric contributions to IRTM T 15 and thus allows the atmospheric component to be estimated. The resulting bias amounts to a ∼15-K offset for midday atmospheric temperatures at subsolar latitudes during relatively clear periods and is negligible at night. The proposed temperature correction results in close agreement between the stimulated and observed patterns of diurnal variation for conditions ranging from clear to dusty.A major consequence of this work is the improved definition of the diurnal, latitudinal, and seasonal variation of martian atmosphere temperatures during the Viking mission. An accounting for the surface temperature bias resolves much of the discrepancy between IRTM and corresponding microwave observations, indicating that there is relatively little interannual variability in global temperatures during the aphelion season (L s ∼ 40• -100 • ). We find further support for this argument in a comparison with T 15 temperatures synthesized from Mariner 9 Infrared Interferometer Spectrometer spectra. The significantly reduced diurnal temperature variations in this season are consistent with the relatively clear atmosphere that is implied by the cooler temperatures. Cooler temperatures and reduced diurnal variation will likely be of significance for the modeling of water ice cloud dynamics in this season.

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Section: Interannual Variability Of Aphelion Season Temperaturesmentioning

confidence: 61%

The Martian Atmosphere During the Viking Mission, I Infrared Measurements of Atmospheric Temperatures Revisited

Wilson¹

2000

Icarus

112

135

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“…• ) with Mars Global Surveyor TES instrument and the Kitt Peak, Arizona, observatory (Clancy et al 2000). The profile we retrieve shows significant warming between 20 and 55 km (up to 20 K compared to the MY24 scenario and 10 K compared to the Warm scenario, in 2005).…”

Section: Discussionmentioning

confidence: 97%

Vertical temperature profile and mesospheric winds retrieval on Mars from CO millimeter observations

Cavalié

Billebaud

Encrenaz

et al. 2008

A&A

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Aims.We have recorded high spectral resolution spectra and derived precise atmospheric temperature profiles and wind velocities in the atmosphere of Mars. We have compared observations of the planetary mean thermal profile and mesospheric wind velocities on the disk, obtained with our millimetric observations of CO rotational lines, to predictions from the Laboratoire de Météorologie Dynamique (LMD) Mars General Circulation Model, as provided through the Mars Climate Database (MCD) numerical tool. Methods. We observed the atmosphere of Mars at CO(1−0) and CO(2−1) wavelengths with the IRAM 30-m antenna in June 2001 and November 2005. We retrieved the mean thermal profile of the planet from high and low spectral resolution data with an inversion method detailed here. High spectral resolution spectra were used to derive mesospheric wind velocities on the planetary disk. We also report here the use of 13 CO(2−1) line core shifts to measure wind velocities at 40 km.

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“…Earth-based observations, which document the recessional behavior of the polar caps and changes in large-scale cloud cover and dust storm activity, have revealed two important attributes of the Martian climate system: that the patterns of large-scale seasonal cap recession reoccur from year to year [Cantor et al, 1998; and that large regional and global dust storms develop more or less randomly during a half year period referred to as the classical ''dust storm season,'' L s = 150°-340° [Martin and Zurek, 1993], where L s is the areocentric longitude of the Sun, measured from 0°at Mars' northern spring equinox. Ground-based millimeter measurements of dayside average atmospheric temperatures in Mars' low to middle latitudes during the 1990s [Clancy et al, 2000] suggested that perihelion regional or global dust storms occur in every Mars year, as suggested by Zurek [1982] .…”

Section: Introductionmentioning

confidence: 99%

Multiyear Mars Orbiter Camera (MOC) observations of repeated Martian weather phenomena during the northern summer season

2002

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[1] The Mars Global Surveyor Mars Orbiter Camera (MGS MOC) has observed several atmospheric events repeat within a few degrees of L s from one year to the next over 3 Mars years during a portion of the northern summer, southern winter seasons (L s = 124°-140°). The repeatability suggests a previously unobserved lack of significant variation in the present Martian northern summer seasonal climate. Nonetheless, interannual variations in the seasonal south polar cap and in the residual north polar cap were observed. These appear to have had a negligible effect in perturbing Mars' weather during the northern summer season.

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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

Cited by 364 publications

References 53 publications

The Martian Atmosphere During the Viking Mission, I Infrared Measurements of Atmospheric Temperatures Revisited

The Martian Atmosphere During the Viking Mission, I Infrared Measurements of Atmospheric Temperatures Revisited

Vertical temperature profile and mesospheric winds retrieval on Mars from CO millimeter observations

Multiyear Mars Orbiter Camera (MOC) observations of repeated Martian weather phenomena during the northern summer season

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