Temperature inversions, thermal tides, and water ice clouds in the Martian tropics

By D. Hinson, Robert J. Wilson. 2003

140 citations recorded by the source corpus.

View Paper: https://www.semanticscholar.org/paper/1587e406ce2eed380c2b8a33e383cd5f7d7f9e7a

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In Astronomy and Astrophysics

Citations in the corpus

Origin and role of water ice clouds in the Martian water cycle as inferred from a general circulation model (2004, methodology): “In what follows we draw heavily from the analysis of [Houben et al., 1997; Richardson and Wilson, 2002] in explaining the seasonal and geographical distribution of water vapor. [41] Overall, our model provides a good match of the observed water cycle. A prominent peak in water vapor occurs over the ”
Evolved Climates and Observational Discriminants for the TRAPPIST-1 Planetary System (2018, background): “This stratospheric absorption induces heating in the atmosphere, exceeding heating at the planetary surface, causing a surface temperature inversion similar to Earth and Mars at night (e.g., André & Mahrt 1982; Hinson & Wilson 2004) and inhibiting a troposphere from forming.”
The influence of radiatively active water ice clouds on the Martian climate (2012, methodology): “Other inversions were later discovered in the equatorial regions during the Ls = 145 –155 period in the radio occultations of MGS (Mars Global Surveyor) and successfully reproduced by implementing the radiative effect of clouds in the GFDL/MGCM [Hinson and Wilson, 2004].”
Spacecraft Observations of the Martian Atmosphere (2008, background): “A few radio occultation profiles show large-amplitude waves (purple profile), which may be caused by the presence of water ice clouds (Hinson & Wilson 2004).”
THE MARTIAN ATMOSPHERIC BOUNDARY LAYER (2011, unknown): “…is highly anisotropic: along the line‐of‐sight the horizontal resolution is of the order of few hundred kilometers, in the direction perpendicular to the line‐of‐sight horizontal resolution is comparable to the vertical resolution [Hinson et al., 1999, 2001, 2004; Hinson and Wilson, 2004].”
MGS Radio Science electron density profiles: Interannual variability and implications for the Martian neutral atmosphere (2004, background): “Detailed analysis of the available neutral temperature profiles of the lower atmosphere is described in several recent papers [e.g., Hinson et al., 1999, 2001, 2003a; Hinson and Wilson, 2002, 2004].”
Revisiting the radiative impact of dust on Mars using the LMD Global Climate Model (2011, methodology): “More recently, Hinson and Wilson [2004], Wilson et al.”
Constraints on dust aerosols from the Mars Exploration Rovers using MGS overflights and Mini‐TES (2006, methodology): “Hunt [1979] and Martin [1986] examine Infrared Thermal Mapper observations obtained near the site with the context of lander data; Clancy and Lee [1991] employ the lander optical depths as a demonstration of the viability of their emission phase function retrieval methodology.”