An intercomparison of ground-based millimeter, MGS TES, and Viking atmospheric temperature measurements: Seasonal and interannual variability of temperatures and dust loading in the global Mars…

By R. Clancy, B. Sandor, Michael J. Wolff, Philip R. Christensen, Michael D. Smith, J. Pearl, B. Conrath, Robert J. Wilson. 2000

394 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Physiology

View Paper: https://www.semanticscholar.org/paper/0df8f48cef61b699ead39846761a1758144ccc85

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Citations in the corpus

High-resolution thermal inertia derived from the Thermal Emission Imaging System (THEMIS): Thermal model and applications (2006, background): “Finally, dust opacity does not vary dramatically spatially, and variations are largely seasonally repeatable from year to year [Clancy et al., 2000; M.D. Smith et al., 2001].”
Spacecraft Observations of the Martian Atmosphere (2008, methodology): “When comparing observations taken during different years, it is useful to use the “Mars Year” numbering system of Clancy et al. (2000), where 11 April 1955 is adopted as the beginning (Ls = 0◦) of Mars Year 1 (MY 1).”
Temperature inversions, thermal tides, and water ice clouds in the Martian tropics (2003, background): “(In this convention for counting Martian years, MY 1 begins at L s = 0° on 11 April 1955 [Clancy et al., 2000]).”
Simulation of the Martian dust cycle with the GFDL Mars GCM (2004, background): “…that it is maintained by slow fallout of dust following global dust storms: the high degree of repeatability of air temperatures in northern spring and summer [Richardson, 1998; Clancy et al., 2000; Liu et al., 2003; Smith, 2004] contrasts sharply with the interannual variability of global storms.”
The High Resolution Stereo Camera (HRSC) of Mars Express and its approach to science analysis and mapping for Mars and its satellites (2016, methodology): “The first HRSC image in orbit around Mars was captured in orbit 8 on January 09, 2004 or at the end of Mars year (MY) 26 following the convention for a Mars calendar as introduced by Clancy et al. (2000).”
Modeling the Martian dust cycle and surface dust reservoirs with the NASA Ames general circulation model (2006, methodology): “3.1. Atmospheric Dust Loading [37] The pattern of zonally averaged 9 mm opacity (scaled to the 6.1 mbar pressure surface) generated in this baseline simulation agrees reasonably well with TES observations during Mars years 24 and 26 (Figure 2; ‘‘Mars year’’ numbering was defined by Clancy et al. [2”
Compact Reconnaissance Imaging Spectrometer for Mars (CRISM) on Mars Reconnaissance Orbiter (MRO) (2007, background): “Global dust storms in this season occur only infrequently but regional dust storms have shown surprising repeatability across different Martian years [Clancy et al., 2000; Smith et al., 2001; Cantor et al., 2002; Smith, 2004].”
One Martian year of atmospheric observations using MER Mini‐TES (2006, background): “The ‘‘Mars Year’’ convention is from Clancy et al. [2000] , where Mars Year 1 begins on 11 April 1955.”
Long-term monitoring of martian gully formation and evolution with MRO/HiRISE (2015, methodology): “We use the Mars calendar of Clancy et al. (2000), in which Mars Year 1 (MY1) began at”
Mapping the methane on Mars (2010, background): “…this spectral region by the thermal emission spectrometer (TES) onboard Mars Global Surveyor (MGS) (Christensen et al. 2001), which provides full spatial coverage of Mars over about three martian years (MYs) (Clancy et al. 2000), i.e. the second half of MY24, MY25, MY26, and the first half of MY27.”