Infrared Spectroscopy Experiment on the Mariner 9 Mission: Preliminary Results

Hanel, Rudolf; Conrath, B. J.; Hovis, W. A.; Kunde, V. G.; Lowman, Paul D.; Pearl, J. C.; Prabhakara, C.; Schlachman, B.; Levin, Gilbert V.

doi:10.1126/science.175.4019.305

Cited by 88 publications

(28 citation statements)

References 15 publications

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“…Due to the fact that the instrument field of view includes both frost covered and clear areas over the Polar caps (Hanel, et al, 1972b), these temperatures are not inconsistent with a CO2 cap. based on an atmospheric scale height of 10 km, and a zero level at the 6.…”

Section: Carbon Dioxide and Water Vapor Transmittancesmentioning

confidence: 99%

“…The scientific goals of the infrared spectroscopy experiment as established in advance of the mission have been discussed (Hanel et al, 1970); a description of the Fourier transform spectrometer used in this experiment has been given (Hanel et al, 1972a); and first results and interpretation of the data up to May 1972 have been published (Hanel et al, 1972b(Hanel et al, , 1972c. The purpose of this paper is to report on analysis of the data carried out from June through October 1972.…”

Section: Introductionmentioning

confidence: 99%

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Atmospheric and surface properties of Mars obtained by infrared spectroscopy on Mariner 9

Conrath¹,

Curran²,

Hanel³

et al. 1973

J. Geophys. Res.

191

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During the almost 1‐year operational lifetime of Mariner 9 the infrared spectroscopy experiment obtained data over a large portion of Mars. Between June and October 1972, improvements were made in the CO2 transmittances, which are necessary for the interpretation of the thermal emission spectra. Recently obtained spectra indicate that strong seasonal variations in the water vapor distribution occurred over both polar regions. The wettest atmospheric conditions observed so far contain 20–30 precipitable μm of water over the north polar cap during northern spring. A low‐resolution pressure map is presented that covers that portion of the planet between latitudes −60° and +25°. A more detailed study of the Coprates canyon indicates that, at its lowest point, the canyon floor must be at least 5km below the rim. Applications of tidal theory to temperature fields derived from the spectra indicate diurnal surface pressure fluctuations of as much as 12% during the Great Dust Storm of 1971–1972. Arguments based on radiative transfer calculations for model dust clouds composed of spherical quartz particles suggest that particle radii during the storm were on the order of a few micrometers; a complete specification of particle parameters must await the development of more refined models.

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Section: Carbon Dioxide and Water Vapor Transmittancesmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Atmospheric and surface properties of Mars obtained by infrared spectroscopy on Mariner 9

Conrath¹,

Curran²,

Hanel³

et al. 1973

J. Geophys. Res.

191

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“…The spectral data were obtained in the range 200 to 2000 cm −1 (5-50 µm) with 2.4 cm −1 resolution (Hanel et al 1972a) enabling us to synthesize an equivalent set of T 15 and T 20 observations (hereafter IRIS T 15 and T 20 ) by convolving the IRIS data with the corresponding IRTM filter response functions. This procedure allows for a direct comparison of IRIS and IRTM results.…”

Section: Comparison Between Irtm and Iris T 15 Temperaturesmentioning

confidence: 99%

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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“…These observations will build upon IR observations collected by previous spacecraft, in particular the Mariner 9 Infrared Interferometer Spectrometer (IRIS) (1,2) and Viking Infrared Thermal Mapper (IRTM) investigations (3,4). The specific objectives of the TES experiment are: (i) to determine and map the composition of surface minerals, rocks, and ices; (ii) to study the composition, particle size, and spatial and temporal distribution of atmospheric dust; (iii) to locate water-ice and CO 2 condensate clouds and determine their temperature, height, and condensate abundance; (iv) to study the growth, retreat, and total energy balance of the polar cap deposits; (v) to measure the thermophysical properties of the martian surface materials; and (vi) to characterize the thermal structure and dynamics of the atmosphere (5).…”

mentioning

confidence: 99%

Results from the Mars Global Surveyor Thermal Emission Spectrometer

Christensen

Anderson

Chase

et al. 1998

Science

Self Cite

196

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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° 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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Infrared Spectroscopy Experiment on the Mariner 9 Mission: Preliminary Results

Cited by 88 publications

References 15 publications

Atmospheric and surface properties of Mars obtained by infrared spectroscopy on Mariner 9

Atmospheric and surface properties of Mars obtained by infrared spectroscopy on Mariner 9

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

Results from the Mars Global Surveyor Thermal Emission Spectrometer

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