The annual cycle of water vapor on Mars as observed by the Thermal Emission Spectrometer

By Michael D. Smith. 2002

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In Astronomy and Astrophysics

Citations in the corpus

Revisiting the radiative impact of dust on Mars using the LMD Global Climate Model (2011, methodology): “(first column) Zonally and time averaged (over 30° of Ls) temperature fields as measured by TES [Smith, 2002] for Martian year 25.”
Constraints on the size of Martian aerosols from Thermal Emission Spectrometer observations (2003, background): “from Smith [2002]. No attempt was made to refine the H2O column or to account for the wavenumber offsets between detectors which will significantly impact the model-data comparison in the 200–350 cm 1 range due to the ‘‘sharpness’’ of the lines [Smith, 2002].”
Compact Reconnaissance Imaging Spectrometer observations of water vapor and carbon monoxide (2009, methodology): “Nevertheless, the CRISM observations can still be put into perspective by comparison against the long record of TES observations of water vapor [ Smith, 2002, 2004, 2008 ].”
Global distribution, composition, and abundance of olivine on the surface of Mars from thermal infrared data (2008, background): “The Fo11–24 index also lacks spatial coherence, and appears to be dominated by highly variable emission features associated with water vapor and ice in the Smith, 2002 ].”
CRISM multispectral summary products: Parameterizing mineral diversity on Mars from reflectance (2007, methodology): “[2006] from the hyperspectral OMEGA data and are consistent with previous ground-based and spacecraft observations [e.g., Jakosky and Farmer, 1982; Smith, 2002; Sprague et al., 2003].”
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 Thermal Emission Spectrometer (TES) onboard the MGS orbiter accumulated almost three Mars years of observations of atmospheric temperature, dust, and water vapor column abundance [Smith et al., 2001; Smith, 2002].”
Interannual variability in TES atmospheric observations of Mars during 1999–2003 (2004, methodology): “Water vapor abundance has a significant positive correlation with surface pressure (topography) and albedo, and a significant negative correlation with thermal inertia ( Smith, 2002 ).”
Geologic Constraints on Early Mars Climate (2018, background): “The modern Mars atmosphere+(ice cap) system has ~34 m Global Equivalent Layer of H2O ice (Carr & Head 2015), 10-5 m Global Equivalent Layer of H2O vapor (Smith 2002), and no liquid water.”
Constraints on dust aerosols from the Mars Exploration Rovers using MGS overflights and Mini‐TES (2006, methodology): “As discussed by Smith et al. [2006], the presence of dust on the Mini-TES optics eventually becomes an issue in terms a ‘‘contamination’’ of the atmospheric radiance.”
Origin and role of water ice clouds in the Martian water cycle as inferred from a general circulation model (2004, methodology): “In particular, we have focused on the model ability to reproduce the observed seasonal evolution of the total amount of water in each hemisphere [ Smith, 2002 ].”
Temperature inversions, thermal tides, and water ice clouds in the Martian tropics (2003, background): “However, the column abundance of water vapor in the tropics remained substantial ( 20 pr-mm) during this interval [Smith, 2002].”
Formation of recurring slope lineae by liquid brines on present‐day Mars (2012, background): “During the favorable season, the maximum water vapor amounts in the atmosphere does not exceed 100 precipitable mm [Smith, 2002].”
One Martian year of atmospheric observations using MER Mini‐TES (2006, methodology): “Smith et al. [2004] previously showed a similar sample of temperature profiles.”
Three-dimensional modeling of ozone on Mars (2004, background): “considerably with latitude and season [Jakosky and Farmer, 1982; Smith, 2002].”
Global mineral distributions on Mars (2002, methodology): “The lack of significant absorption in moderate- to low-albedo regions at 1500 cm 1 in TES spectra with minor CO2 and water vapor absorptions removed may be used to limit carbonate concentrations to significantly less than 0.10 [Bandfield and Smith, 2001; Christensen et al., 2001a].”
Compact Reconnaissance Imaging Spectrometer for Mars (CRISM) on Mars Reconnaissance Orbiter (MRO) (2007, background): “Atmospheric H2O vapor varies in abundance seasonally, with greatest abundance ( 100 pr-mm) in summertime at northern high latitudes [Jakosky and Farmer, 1982; Smith, 2002, 2004].”