Kinetic Calculations of the Charge Exchange Efficiency for Solar Wind Protons in the Extended Martian Hydrogen Corona

Abstract

Model calculations of the charge exchange efficiency for solar wind protons colliding with hydrogen atoms of the extensive Martian corona are presented. It is shown that the energy spectrum of hydrogen atoms penetrating in the Martian atmosphere is identical to the spectrum of protons of the unperturbed solar wind. The charge exchange efficiency varies from 2 to 4% depending on the boundary location of the Martian induced magnetosphere. The presented calculations, combined with the kinetic model of proton precipitation proposed earlier, enable us to follow all proton penetration stages of the unperturbed solar wind into denser atmospheric layers and to estimate the characteristics of proton aurorae observed on the Mars.