Effect of Variations in the Extended Hydrogen Corona of Mars on the Efficiency of Charge Exchange with Solar Wind Protons
| Autor: | Andrey Zhilkin, D. V. Bisikalo, V. I. Shematovich |
|---|---|
| Rok vydání: | 2021 |
| Předmět: |
Physics
Martian Proton 010308 nuclear & particles physics Astronomy and Astrophysics Atmosphere of Mars Mars Exploration Program 01 natural sciences Corona Computational physics Atmosphere Solar wind Space and Planetary Science Physics::Space Physics 0103 physical sciences Astrophysics::Solar and Stellar Astrophysics Astrophysics::Earth and Planetary Astrophysics 010303 astronomy & astrophysics Physics::Atmospheric and Oceanic Physics Water vapor |
| Zdroj: | Astronomy Reports. 65:203-208 |
| ISSN: | 1562-6881 1063-7729 |
| DOI: | 10.1134/s1063772921030033 |
| Popis: | This paper presents the results of calculating the efficiency of solar wind proton charge exchange as a function of variations in the column density of hydrogen atoms in the extended corona of Mars. The presence of regular density variations has been known for a long time and has been associated with the change of seasons on Mars. However, sporadic density variations in the upper Martian atmosphere were detected recently as well. They were caused by various processes in the underlying atmosphere, such as ejection of water vapor and ice particles at altitudes up to 100 km due to global dust storms, which was discovered in the Mars Express and MAVEN observations. Taking into account the variations in the column density with the observed amplitude up to one order of magnitude is absolutely necessary to correctly consider the interaction of solar wind protons with the Martian atmosphere. The calculations using the kinetic Monte Carlo model revealed that with a 2- and 5-fold increase in the column density of H atoms in the corona of Mars, the charge exchange efficiency also increases and reaches 6% and 8%, respectively, as compared to the base value of 4%. The energy spectrum of hydrogen atoms penetrating into the Martian atmosphere does not change and remains identical in structure to the spectrum of undisturbed solar wind protons. These estimates, combined with the previously developed kinetic model of the proton and hydrogen atom precipitation into the planetary atmosphere, make it possible to do the following: to trace all the stages of the penetration of the undisturbed solar wind protons into the dense layers of the atmosphere, as well as interpret the observed characteristics of proton auroras depending on the variations of atomic hydrogen content in the Martian corona. |
| Databáze: | OpenAIRE |
| Externí odkaz: |
|