3D NUMERICAL MODEL FOR STUDYING ELECTRON PRECIPITATION IN THE UPPER ATMOSPHERES OF VENUS-LIKE EXOPLANETS

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Abstract

The paper presents a three-dimensional numerical model of solar wind plasma flow around a terrestrial planet that does not have its own magnetic field. The model is based on the approximation of multicomponent magnetohydrodynamics and takes into account ionization and recombination processes. The numerical model is validated using the example of the magnetosphere of Venus. Our model, in particular, allows us to calculate the structure and parameters of electron precipitation into the planet’s ionosphere. The developed model is supposed to be used to study observational manifestations of the potential biomarker NO in the atmospheres of exoplanets without their own magnetic field.

About the authors

A. G Zhilkin

Institute of Astronomy of the Russian Academy of Sciences

Email: zhilkin@inasan.ru
Moscow, Russia

V. I Shematovich

Institute of Astronomy of the Russian Academy of Sciences

Moscow, Russia

G. N Tsurikov

Institute of Astronomy of the Russian Academy of Sciences

Moscow, Russia

D. V Bisikalo

Institute of Astronomy of the Russian Academy of Sciences; National center of physics and mathematics

Moscow, Russia; Sarov, Russia

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