Simulation Results for Effects of Global and Regional Dust Storms on the Martian Hot O Corona and Photochemical Loss
Description of this data
We examine here for the first time the effects of both global and regional dust storms on the formation of the Martian hot O corona and associated photochemical loss of O. Our study is conducted by utilizing our integrated model framework, which couples our Martian hot O corona model with a multifluid magnetohydrodynamic model for Mars for the dusty and clear atmospheric condition cases. We present our results with the most up-to-date cross sections for the O(3P)-CO2 collisions. The main effect of dust storms on the ionosphere is the upward shift of the ionosphere on the dayside, which results in an increase in production of hot O at all altitudes above the ionospheric peak. However, the dust-induced inflation of the neutral upper atmosphere results in an enhancement in collisional loss of hot O and thus effectively suppresses the hot O density, reducing the global photochemical loss rate by ~28% for the global dust storm scenario. The relative density structure of the hot O corona does not show any significant changes, while its magnitude decreases at all altitudes.
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Cite this dataset
Lee, Yuni (2019), “Simulation Results for Effects of Global and Regional Dust Storms on the Martian Hot O Corona and Photochemical Loss”, Mendeley Data, v1 http://dx.doi.org/10.17632/c85kp386fd.1
The files associated with this dataset are licensed under a Creative Commons Attribution 4.0 International licence.