Investigation of the Martian environment by infrared spectroscopy on Mariner 9

Hanel, Rudolf; Conrath, B. J.; Hovis, W. A.; Kunde, V. G.; Lowman, Paul D.; Maguire, W. C.; Pearl, J. C.; Pirraglia, J. A.; Prabhakara, C.; Schlachman, B.; Levin, Gilbert V.; Straat, Patricia Ann; Burke, T. E.

doi:10.1016/0019-1035(72)90009-7

Cited by 320 publications

(118 citation statements)

References 34 publications

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“…The measured abundance increased slightly at the end of the favorable Doppler shift to the 15gm level at an L s of 355 ° . The ground-based measurements over this period agreed quite well with the in situ measurements made by the IRIS instrumentation (Hanel et al, 1972) aboard the Mariner 9 spacecraft. A few additional ground-based observations of less than 10gin were obtained at L s values of 15 and 21 ° with a very small planet.…”

supporting

confidence: 75%

“…12 we show the vertical temperature profiles determined by Mariner 9 (Hanel et al, 1972 ;Conrath, 1974, personal communication) for a similar season and subsolar latitude as the ground-based water vapor studies. The profiles are for the local times of the maximum and minimum H20 abundances for both the morning and evening terminator series for an assumed -3°/km lapse rate.…”

mentioning

confidence: 88%

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Martian atmospheric water vapor observations: 1972–1974 apparition

Barker¹

1976

Icarus

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The patrol of Martian water vapor carried out with the echelle-coudil scanner at McDonald Observatory during the 1972-74 apparition has produced 469 individual photoelectric scans of Doppler-shifted Martian H20 lines. Almost an entire Martian year was covered during the 1972-74 period (L s = 118-269 ° and 301-80°). Three types of coverage have been obtained : ( 1 ) regular--the slit placed pole to pole on the central meridian; (2) latitudinal--the slit placed parallel to the Martian equator at various latitudes; (3) diurnal--the slit placed parallel to the terminator at several times during a Martian day measured from local noon.Both the seasonal and diurnal effects seem to be controlled by the insolation and not the local topography with respect to the 6.1 mb surface. A slight negative correlation with elevation was noted which improved during the seasons of greater H20 content. The previous seasonal behavior has been confirmed and amplified. The following are the primary conclusions: (1) The planetwide abundance is low (5-15~m of ppt H20 ) during both equinoctical periods. (2) The maximum abundance of about 40~am occurs in each hemisphere after solstice at about 40 ° latitude in that hemisphere. (3) The latitude of the maximum amount in the N-S distribution precedes the latitude of maximum insolation by 10-20 ° of latitude. (4) During the "drier" seasons (5-20~m) near the equinoxes on Mars, the atmospheric water vapor changes by a factor of 2-3 × over a diurnal cycle with the maximum near local noon. (5) The effects of the 1973 dust storm during the southern summer reduced the amount of water vapor over the southern hemisphere regions to 3-81zm. INTRODUCTIOI~ AI~D HISTORY

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supporting

confidence: 75%

mentioning

confidence: 88%

Martian atmospheric water vapor observations: 1972–1974 apparition

Barker¹

1976

Icarus

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“…Mariner 9 Infrared Interferometer Spectrome ter (IRIS) observations of the cold spots provided high resolution (2.4 cm-l ) spectral information [Hanel et al, 1972]. The characteristic spectral feature of these cold spots was a broad band decrease in the brightness tem perature around 25 J.Lm, or equivalently, a decrease in the CO2 emissivity owing to volume scattering.…”

Section: Prior Observationsmentioning

confidence: 99%

TES premapping data: Slab ice and snow flurries in the Martian north polar night

Titus¹,

Kieffer²,

Mullins³

et al. 2001

J. Geophys. Res.

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“…For example, data obtained by the Mariner 9 Infrared Interferometer Spectrometer (IRIS) instrument during the 1971 global dust storm indicate a strong diurnal temperature variation (∼30 K peak-to-peak) in the summer hemisphere, extending to at least 40 km (Hanel et al 1972b). Comparable diurnal temperature variations (at ∼25 km) are evident in the IRTM T 15 data following the onset of the 1977a and 1977b dust storms .…”

Section: Introductionmentioning

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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Investigation of the Martian environment by infrared spectroscopy on Mariner 9

Cited by 320 publications

References 34 publications

Martian atmospheric water vapor observations: 1972–1974 apparition

Martian atmospheric water vapor observations: 1972–1974 apparition

TES premapping data: Slab ice and snow flurries in the Martian north polar night

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

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