Observations of water vapour anomaly above Tharsis volcanoes on Mars in the ISM (Phobos-2) experiment

Titov, D. V.; Мороз, В. І.; Grigoriev, Аlexey; Rosenqvist, J.; Combes, M.; Bibring, Jean‐Pierre; Arnold, G.

doi:10.1016/0032-0633(94)90060-4

Cited by 25 publications

(10 citation statements)

References 25 publications

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“…The Infrared Imaging Spectrometer (ISM) on board the Phobos-2 mission has shown a variability in water vapor abundance between morning and noon of a factor of 2-3 in the Pavonis Mons region (Titov et al, 1994); a re-analysis of the IRIS/Mariner-9 data set by Formisano et al (2001) also indicated a variability in day/night time water vapor abundance of about a factor of two, in an anticorrelation with dust opacity.…”

Section: Local Time Variationsmentioning

confidence: 96%

Mars’ water vapor mapping by the SPICAM IR spectrometer: Five martian years of observations

Trokhimovskiy

Fedorova

Korablev

et al. 2015

Icarus

101

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Section: Local Time Variationsmentioning

confidence: 96%

Mars’ water vapor mapping by the SPICAM IR spectrometer: Five martian years of observations

Trokhimovskiy

Fedorova

Korablev

et al. 2015

Icarus

101

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“…driven by solar forcing, and an efficient mixing within the boundary layer due to convection and turbulent eddies. The time scale of eddy mixing is given by τ = H (z) 2 / (z) with the scale height H (z) and the eddy mixing coefficient (z) which are both a function of height (Titov et al, 1994). Within the boundary layer the coefficient is ≈ 10 7 -10 8 cm 2 s −1 while in the atmosphere above it is ≈ 10 6 cm 2 s −1 .…”

Section: Vertical Distributionmentioning

confidence: 99%

Investigation of water vapor on Mars with PFS/SW of Mars Express

Tschimmel

Ignatiev

Титов

et al. 2008

Icarus

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“…The maps of atmospheric water vapor distribution retrieved from these data revealed spatial variations of up to a factor of 5 correlated with topography and surface albedo. Significant diurnal variations were also observed [Titov et al, 1994 …”

Section: Introductionmentioning

confidence: 95%

Measurements of the atmospheric water vapor on Mars by the Imager for Mars Pathfinder

Титов¹,

Markiewicz²,

Thomas³

et al. 1999

J. Geophys. Res.

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Abstract. The Imager for Mars Pathfinder (IMP) was the first instrument to measure the atmospheric water on Mars from its surface. It took the images of the Sun through the Martian atmosphere in five narrowband filters, two in the 0.94 gm H20 band and three in the continuum around it. The observations were carried out in the mornings and in the evenings when the Sun was between 3 ø and 8 ø above the horizon. The absorption due to the atmospheric water vapor did not exceed 2%. An average column density of 6_+4 precipitated microns (pr gm) was derived from the IMP data. The dependence of the observed 1-120 transmittance on Sun elevation tentatively implies that the water vapor is not uniformly mixed in the atmosphere but is rather confined to a layer 1-3 km thick near the surface. IMP observations also indicate a horizontal inhomogeneity of the layer but show no significant morning-to-evening variations of the water vapor amount.

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Observations of water vapour anomaly above Tharsis volcanoes on Mars in the ISM (Phobos-2) experiment

Cited by 25 publications

References 25 publications

Mars’ water vapor mapping by the SPICAM IR spectrometer: Five martian years of observations

Mars’ water vapor mapping by the SPICAM IR spectrometer: Five martian years of observations

Investigation of water vapor on Mars with PFS/SW of Mars Express

Measurements of the atmospheric water vapor on Mars by the Imager for Mars Pathfinder

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