Thermal Emission Spectrometer Observations of Martian Planet-Encircling Dust Storm 2001A

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

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In Astronomy and Astrophysics

Citations in the corpus

SEVEN-YEAR WILKINSON MICROWAVE ANISOTROPY PROBE (WMAP) OBSERVATIONS: PLANETS AND CELESTIAL CALIBRATION SOURCES (2010, background): “The first WMAP Mars observing season occurred during the time of the 2001 July-October massive global dust storm which elevated atmospheric temperatures in the mid-IR by nearly 40 K (Smith et al. 2002).”
Interannual variability in TES atmospheric observations of Mars during 1999–2003 (2004, background): “Second is the heating of the atmosphere in response to dust storms (compare with Fig. 5). The largest examples are at Ls = 225◦ and 260◦ during MY 24 and at Ls = 185◦ during MY 25. The largest dust storm (MY 25, Ls = 185◦) caused atmospheric temperatures at 0.5 mbar to rise by more than 40 K over a ”
Global climate modeling of the Martian water cycle with improved microphysics and radiatively active water ice clouds (2013, result): “As mentioned above, this situation is not realistic, as observations by the MGS Mars Orbiter Camera [Wang and Ingersoll, 2002] or TES [Smith et al., 2002] show that clouds above the Northern polar cap during summer are intermittent, scattered across the polar region and very faint.”
One Martian year of atmospheric observations using MER Mini‐TES (2006, background): “These observations are consistent with TES observations [ Smith et al., 2002, 2004 ], which show that while the heating effect of a dust storm can be tens of degrees above 20 km height, it is minimal in the lowest scale height.”
Constraints on the size of Martian aerosols from Thermal Emission Spectrometer observations (2003, methodology): “[37] Toward study of the dust temporal evolution, we construct a sample comprised of three small regions for a constant longitude range: a rectangle with dimensions 251 –259 Wand 12 –8 S, which is northeast of the storm initiation point [Smith et al., 2002]; and two regions further”
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).”
Compact Reconnaissance Imaging Spectrometer observations of water vapor and carbon monoxide (2009, background): “CRISM water vapor coincides with the onset of the 2007 planet-encircling dust storm (see Figure 3). An artifact in the TES water vapor retrievals caused by the 2001 planetencircling dust storm [ Smith et al., 2002 ] can be seen in the form of lower water vapor abundances during Mars Year 25 between ”
Simulation of the Martian dust cycle with the GFDL Mars GCM (2004, background): “The most dramatic example of such feedback is the Martian global dust storm, which over a matter of weeks can completely enshroud the planet with haze [Leovy et al., 1972; Briggs et al., 1979; Martin and Richardson, 1993; Smith et al., 2002].”
Observations of the initiation and evolution of the 2001 Mars global dust storm (2005, background): “[52] The evolution of dust optical depth can be quantified from the TES thermal spectra and suggests that the storm obtained peak opacities around Ls = 210 [Smith et al., 2002].”
Spacecraft Observations of the Martian Atmosphere (2008, background): “The last two such planet-encircling dust storms erupted in 2001 and 2007 (Smith et al. 2002, Cantor 2007), and it can take a couple months for the dust to settle out back to a nominal level (Conrath 1975).”