Observations of Martian ice clouds by the Mars Global Surveyor thermal emission spectrometer: The first Martian year

John C. Pearl, Michael D. Smith, Barney J. Conrath, Joshua L. Bandfield, Philip Christensen

Research output: Contribution to journalArticle

106 Citations (Scopus)

Abstract

Successful operation of the Mars Global Surveyor spacecraft, beginning in September 1997 (Ls = 184°), has permitted extensive observations over more than a Martian year. Initially, thin (normal optical depth <0.06 at 825 cm-1) ice clouds and hazes were widespread, showing a distinct latitudinal gradient. With the onset of a regional dust storm at Ls = 224°, ice clouds vanished in the southern hemisphere, to reappear gradually after the decay of the storm. The zonally averaged cloud opacities show little difference between the beginning and end of the first Martian year. A broad low-latitude cloud belt with considerable longitudinal structure was present in early northern summer. Apparently characteristic of the northern summer season, it vanished between Ls = 140° and 150°. The latitudinal extent of this feature is apparently controlled by the ascending branch of the Hadley circulation. The most opaque clouds (optical depth ∼0.6) were found above the summits of major volcanic features; these showed spatial structure possibly associated with wave activity. Variety among low-lying late morning clouds suggests localized differences in circulation and microclimates. Limb observations showed extensive optically thin (optical depth <0.04) stratiform clouds at altitudes up to 55 km. Consederable latitude and altitude variations were in ice clouds in early northern spring (Ls = 25°); near 30 km, thin clouds extended from just north of the equator to ∼45°N, nearly to the north polar vortex. A water ice haze was present in the north polar night (Ls = 30°) at altitudes up to 40 km. Because little dust was present this probably provided heterogeneous nucleation sites for the formation of CO2 clouds and snowfall at altitudes below ∼20 km, where atmospheric temperatures dropped to the CO2 condensation point. The relatively invariant spectral shape of the water ice cloud feature over space and time indicates that ice particle radii are generally between 1 and 4 μm.

Original languageEnglish (US)
Pages (from-to)12325-12338
Number of pages14
JournalJournal of Geophysical Research E: Planets
Volume106
Issue number6
StatePublished - 2001

Fingerprint

ice clouds
Mars Global Surveyor
Ice
thermal emission
Spectrometers
Mars
spectrometer
spectrometers
ice
optical thickness
haze
optical depth
summer
dust storms
Dust
atmospheric temperature
morning
Southern Hemisphere
equators
Hot Temperature

ASJC Scopus subject areas

  • Oceanography
  • Astronomy and Astrophysics
  • Atmospheric Science
  • Space and Planetary Science
  • Earth and Planetary Sciences (miscellaneous)
  • Geophysics
  • Geochemistry and Petrology

Cite this

Observations of Martian ice clouds by the Mars Global Surveyor thermal emission spectrometer : The first Martian year. / Pearl, John C.; Smith, Michael D.; Conrath, Barney J.; Bandfield, Joshua L.; Christensen, Philip.

In: Journal of Geophysical Research E: Planets, Vol. 106, No. 6, 2001, p. 12325-12338.

Research output: Contribution to journalArticle

Pearl, John C. ; Smith, Michael D. ; Conrath, Barney J. ; Bandfield, Joshua L. ; Christensen, Philip. / Observations of Martian ice clouds by the Mars Global Surveyor thermal emission spectrometer : The first Martian year. In: Journal of Geophysical Research E: Planets. 2001 ; Vol. 106, No. 6. pp. 12325-12338.
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