Observations of Martian ice clouds by the Mars Global Surveyor Thermal Emission Spectrometer: The first Martian year

By J. Pearl, Michael D. Smith, B. Conrath, J. Bandfield, Philip R. Christensen. 2001

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In Astronomy and Astrophysics

Citations in the corpus

Mars aerosol studies with the MGS TES emission phase function observations: Optical depths, particle sizes, and ice cloud types versus latitude and solar longitude (2003, methodology): “The specific angular, seasonal, and spatial coverages of the TES EPF observations evolved over the MGS primary mission.”
The Thermal Emission Imaging System (THEMIS) for the Mars 2001 Odyssey Mission (2004, methodology): “…extends the systematic monitoring of temperature, dust, and water-ice clouds in the martian atmosphere begun by the Mariner 9 IRIS (Conrath et al., 1973), Viking IRTM (Kieffer et al., 1977; Martin, 1986), and TES investigations (Conrath et al., 2000; Smith et al., 2001a, 2002; Pearl et al., 2001).”
Constraints on the size of Martian aerosols from Thermal Emission Spectrometer observations (2003, background): “…works [e.g., Clancy and Lee, 1991; Murphy et al., 1993; Clancy et al., 1995; Pollack et al., 1995; Ockert-Bell et al., 1997; Tomasko et al., 1999, and references therein], while work on water ice is somewhat less voluminous [e.g., Pearl et al., 2001; Glenar et al., 2003, and references therein].”
Global distribution, composition, and abundance of olivine on the surface of Mars from thermal infrared data (2008, methodology): “[10] We selected TES spectra for this study using specific quality criteria including derived surface temperatures >250 K, emission angles Pearl et al., 2001 ].”
Investigation of the nature and stability of the Martian seasonal water cycle with a general circulation model (2002, background): “Sampling from the three Viking years show this signal to be robust, as do terrestrial observations [Jakosky and Barker, 1984; Sprague et al., 1996] and more recently, analysis of MGS Thermal Emission Spectrometer (TES) data [Smith, 2002].”
Bright and dark regions on Mars: Particle size and mineralogical characteristics based on thermal emission spectrometer data (2002, background): “Although water-ice clouds are known to form in an equatorial belt during part of the year [Pearl et al., 2001], there is no evidence for them in the global map.”
Temperature inversions, thermal tides, and water ice clouds in the Martian tropics (2003, background): “[43] The results in Figure 6a are generally consistent with the distribution of water ice clouds observed at the same local time by TES [Smith, 2004, Figure 16; Pearl et al., 2001, Plate 2] and by the MGS Mars Orbiter Camera Table 1.”
Spacecraft Observations of the Martian Atmosphere (2008, methodology): “Water ice clouds are observed to take on many forms including topographically induced clouds, ground fogs, vast polar hoods, and a low-latitude belt of clouds that forms during the aphelion season between Ls = 40◦–140◦ (Anderson & Leovy 1978, Kahn 1984, Clancy et al. 1996, Pearl et al. 2001).”