Interannual variability in TES atmospheric observations of Mars during 1999–2003

By Michael D. Smith. 2004

852 citations recorded by the source corpus.

Subfields: Aerospace Engineering, Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/eec6ef9c320c2ce55e02240cb0f0ab045eb713ff

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Citations in the corpus

Revisiting the radiative impact of dust on Mars using the LMD Global Climate Model (2011, methodology): “…predicted by the LMD/GCM when using the dust radiative properties of Ockert‐Bell et al. [1997] and Forget [1998] on the one hand, and the more recent optical indices of Wolff et al. [2006, 2009] on the other, are analyzed in section 3 and compared to the TES temperature measurements [Smith, 2004].”
Compact Reconnaissance Imaging Spectrometer for Mars (CRISM) on Mars Reconnaissance Orbiter (MRO) (2007, methodology): “In addition, such retrievals will form the basis of atmospheric ‘‘correction’’ re-processing for the multispectral survey (initial processing will be done with climatological data based on observations from MGS TES [Smith, 2004]).”
Global thermal inertia and surface properties of Mars from the MGS mapping mission (2005, methodology): “…re ties s in e inhey bly, ut bove acf re to rtia me diswith eate and ethe ious sion en he bout aps mb ds in the of xrsis perller ners the dis the tian elevation, consistent with average TES spectral observa during much of the mapping mission(Mellon et al., 2000; Smith et al., 2001b; Smith, 2004).”
Structure and dynamics of the Martian lower and middle atmosphere as observed by the Mars Climate Sounder: Seasonal variations in zonal mean temperature, dust, and water ice aerosols (2010, positive): “atmosphere provided by nadir infrared spectroscopy [Smith et al., 2001; Smith, 2004], from which an extensive climatology has been developed, and radio occultation [Hinson et”
Planetary Spectrum Generator: An accurate online radiative transfer suite for atmospheres, comets, small bodies and exoplanets (2018, methodology): “f pressure, temperature, CO 2, N 2, O 2, CO, H 2O, dust, dust size, water ice and ice particle size from the MCD database, while the surface albedo information is determined from the MGS/TES database [40]. 3.3 Gas giants / Dense and hazy atmospheres Planets in which their atmospheres are so thick, t”
Mars Climate Sounder limb profile retrieval of atmospheric temperature, pressure, and dust and water ice opacity (2009, background): “Furthermore the atmosphere does not show much year-to-year variability at this latitude and season [Smith, 2004].”
Detection of methane in the martian atmosphere: evidence for life? (2004, methodology): “Using MGS/TES observations at the same martian season (Smith, 2004), we found that the mean atmospheric temperature very close to 200 K in our field of view at a level of 3 mb (half total pressure).”
Simulation of the Martian dust cycle with the GFDL Mars GCM (2004, background): “Dust opacities have been directly measured from these same orbital platforms [Martin, 1986; Fenton et al., 1997; Smith et al., 2001; Liu et al., 2003; Smith, 2004] and for more limited periods from the ground [Colburn et al., 1989; see also Toigo and Richardson, 2000; Smith and Lemmon, 1999].”
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.”
Global climate modeling of the Martian water cycle with improved microphysics and radiatively active water ice clouds (2013, methodology): “…, 1982] and later monitored for several years by the Thermal Emission Spectrometer (TES) onboard Mars Global Surveyor (MGS) [ Smith et al. , 2001; Smith , 2004], as well as the Mars Express instruments [ Fedorova et al. , 2006; Fouchet et al. , 2007; Tschimmel et al. , 2008; Maltagliati et al.…”
The Atmospheric Chemistry Suite (ACS) of Three Spectrometers for the ExoMars 2016 Trace Gas Orbiter (2018, methodology): “Previous satellite experiments have demonstrated the importance of global mapping at all seasons to pinpoint the sources, sinks, and processes controlling the distribution of water vapor, dust (Smith 2004) or O3 (Perrier et al. 2006).”
Mars Climate Sounder: An investigation of thermal and water vapor structure, dust and condensate distributions in the atmosphere, and energy balance of the polar regions (2007, background): “The TES retrievals ignore these climatological changes, having determined they introduce negligible errors [Smith, 2004].”
Selection of the Mars Science Laboratory Landing Site (2012, methodology): “The models were constrained by and validated against data sets from orbital imaging and sounding (thermal and radio) instruments, which were substantially improved over earlier mission atmospheric characterization efforts by the long history of TES and THEMIS thermal observations (Smith 2004) and th”
Modeling the Martian dust cycle and surface dust reservoirs with the NASA Ames general circulation model (2006, background): “The spatial pattern of surface albedo has been observed to change on subannual timescales [Lee, 1987; Smith, 2004; Kahre et al., 2005a] due to the redistribution of surface dust.”