Thermal structure and dust loading of the Martian atmosphere during late southern summer: Mariner 9 revisited

Santee, M. L.; Crisp, David

doi:10.1029/92je01896

Cited by 71 publications

(35 citation statements)

References 43 publications

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“…We suggest that the negative meridional temperature gradient at tropical latitudes in the 0200 LT figure (Fig. 12b of Santee and Crisp 1993) is an artifact of the erroneous data corresponding to high emission angles. We conclude that the IRIS data are not inconsistent with the diurnal temperature variations suggested by tide modeling.…”

Section: Comparison Between Irtm and Iris T 15 Temperaturesmentioning

confidence: 93%

“…For example, the indicated closing off of the late-afternoon 0.5-mb temperature contours in the southern extratropics is a consequence of the technique used to extrapolate the data. Haberle et al (1993) compared a 1400 LT, 0200 LT difference height-latitude section from the NASA Ames Mars GCM with that derived by Santee and Crisp (1993). The Ames MGCM results ( Fig.…”

Section: Comparison Between Irtm and Iris T 15 Temperaturesmentioning

confidence: 99%

“…The zonal-mean temperature and zonal wind fields are characterized by relatively cool polar latitudes and associated midlatitude westerlies (Santee andCrisp 1993, Haberle et al 1993). The LTM calculation employs a uniformly mixed aerosol distribution (to 35 km) with a column optical depth of FIG.…”

Section: Linear Tidal Model Experimentsmentioning

confidence: 99%

“…It should be noted, however, that the contours in Figs. 11 and 12d of Santee and Crisp (1993) have been extended into regions with poor or no data coverage. For example, the indicated closing off of the late-afternoon 0.5-mb temperature contours in the southern extratropics is a consequence of the technique used to extrapolate the data.…”

Section: Comparison Between Irtm and Iris T 15 Temperaturesmentioning

confidence: 99%

“…19 and with the reprocessed IRTM temperatures. Santee and Crisp (1993) used IRIS spectra to simultaneously retrieve temperature profiles and dust optical depth for the L s = 343…”

Section: Comparison Between Irtm and Iris T 15 Temperaturesmentioning

confidence: 99%

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

Wilson¹

2000

Icarus

113

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: Comparison Between Irtm and Iris T 15 Temperaturesmentioning

confidence: 93%

Section: Comparison Between Irtm and Iris T 15 Temperaturesmentioning

confidence: 99%

Section: Linear Tidal Model Experimentsmentioning

confidence: 99%

Section: Comparison Between Irtm and Iris T 15 Temperaturesmentioning

confidence: 99%

“…19 and with the reprocessed IRTM temperatures. Santee and Crisp (1993) used IRIS spectra to simultaneously retrieve temperature profiles and dust optical depth for the L s = 343…”

Section: Comparison Between Irtm and Iris T 15 Temperaturesmentioning

confidence: 99%

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

Wilson¹

2000

Icarus

113

135

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Characterization of middle‐atmosphere polar warming at Mars

et al. 2013

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[1] We characterize middle-atmosphere polar warming (PW) using nearly three Martian years of temperature observations by the Mars Climate Sounder. We report the observed structure of PW and share hypotheses as to possible explanations, which have yet to be tested with global dynamical models. In the data, PW manifested between p = 15 Pa and p = 4.8Â10 -3 Pa. The latitude where PW maximized shifted poleward with decreasing pressure. The nightside magnitude was larger than the dayside magnitude. The maximum nightside magnitudes ranged from 22 to 67 K. As expected, the annual maximum magnitude in the north occurred during late-local fall to middle-local winter. In the south it occurred during late-local winter. Also as expected, the maximum magnitude near MY 28's southern winter solstice was smaller than that at that same year's northern winter solstice, when a global dust storm was occurring. Unexpectedly, the maximum magnitude at southern winter solstice was comparable to that at northern winter solstice for both MY 29 and MY 30, years that did not experience global dust storms but certainly experienced greater dust loading during L s = 270 than L s = 90 . Another unexpected result was a hemispheric asymmetry in PW magnitude during most of the observed equinoxes. This paper also provides tables of (1) averaged temperatures as a function of latitude, pressure, and season, and (2) the maximum polar warming features as a function of pressure and season. These tables can be used to validate GCM calculations of middle-atmosphere temperatures and constrain calculations of unobserved winds.

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Feasibility of Determining the Composition of Planetary Ices by Far Infrared Observations: Application to Martian Cloud and Surface Ices

Johnson¹,

Atreya²

1996

Icarus

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Thermal structure and dust loading of the Martian atmosphere during late southern summer: Mariner 9 revisited

Cited by 71 publications

References 43 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

Characterization of middle‐atmosphere polar warming at Mars

Feasibility of Determining the Composition of Planetary Ices by Far Infrared Observations: Application to Martian Cloud and Surface Ices

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