Numerical Model to Study Proton Polar Aurorae on Mars

• Published in: Astronomy reports Vol. 66; no. 3; pp. 245 - 254
• Main Authors: Zhilkin, A. G., Bisikalo, D. V., Shematovich, V. I.
• Format: Journal Article
• Language: English
• Published: Moscow Pleiades Publishing 01.03.2022; Springer Nature B.V
• Subjects: Astronomy; Auroras; Daytime; Energy spectra; Fluid flow; Hydrogen; Hydrogen atoms; Jupiter; Magnetic fields; Magnetic properties; Magnetism; Magnetohydrodynamics; Magnetospheres; Mars; Mars atmosphere; Mars missions; Mars spacecraft; Mathematical models; Modelling; Monte Carlo simulation; Numerical models; Observations and Techniques; Parameters; Physics; Physics and Astronomy; Planetary magnetic fields; Proton flux; Protons; Saturn; Solar wind; Solar wind parameters; Spacecraft; Upper atmosphere; MHD; Mars; detached shock wave; ionosphere; solar wind interaction
• ISSN: 1063-7729; 1562-6881
• DOI: 10.1134/S1063772922030076

— We present a hybrid model and a magnetohydrodynamic (MHD) one for the solar wind plasma flow around Mars, which serve to calculate the flux of protons of the solar wind and the boundary of the induced magnetosphere. These parameters are used as input data for the kinetic Monte-Carlo model of the impact of a proton flux of the undisturbed solar wind on the daytime atmosphere of Mars. This model is intended to be used to determine the energy fluxes and the energy spectra of hydrogen atoms penetrating into the daytime upper atmosphere through the induced magnetosphere boundary. The obtained characteristics allow us to estimate the parameters of proton auroral phenomena, which were recently discovered in the upper atmosphere of Mars. Based on these characteristics, proton aurorae, which were observed with the Imaging UV Spectrograph (IUVIS) onboard the Mars Atmosphere and Volatile Evolution (MAVEN) spacecraft, can be calculated. The comparison of the results of these calculations with the observed characteristics opens up a unique opportunity to specify more accurately the properties of the atmosphere and the magnetic field of Mars, as well as enlarges a range of techniques used to determine the solar wind parameters.