Dynamical Heating in the Martian Thermosphere  Journal Article uri icon



  • Dynamical heating and cooling are prominent features of planetary; atmospheres resulting in thermospheric structures on Venus, Earth and; Mars. The purpose of this study is to determine the location and; amplitude of localized heating regions in the Martian thermosphere,; confirm that they occur in regions of wind convergence, and to compare; the observed dynamical heating with that predicted by a global; thermospheric model. This investigation uses several years of data from; the NASA Mars Atmosphere and Volatile EvolutioN (MAVEN) mission; including observations made by the Neutral Gas and Ion Mass Spectrometer; (NGIMS) as well as the Extreme Ultraviolet Monitor (EUVM). Specifically,; the analysis focuses on several years of horizontal wind, temperature,; and composition data. EUVM measurements provide a solar forcing context; for the neutral thermosphere datasets and aid in the statistical; analysis. Statistical results are compared with two versions of the Mars; Global Ionosphere Thermosphere (M-GITM) global circulation model; one; that that includes gravity wave parametrization and a version without; gravity wave effects. Data analysis indicates that heating features; exists around 2-3 and 17-18 local solar time. These locations coincide; with regions of converging winds and are in better agreement with M GITM; when gravity wave parametrization is included in the model. A migrating; oscillation in the observed wind field also results in convergence and a; density enhancement near 15 local time. While a similar oscillation is; reproduced by the model, the amplitude is much lower than observed and; may be a result of modeled zonal winds that are too low.

publication date

  • December 11, 2022

has restriction

  • green

Date in CU Experts

  • December 20, 2022 8:21 AM

Full Author List

  • Pilinski M; Roeten KJ; Bougher SW; Benna M

author count

  • 4

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