Model of the tail region of the heliospheric interface

Details Model of the tail region of the heliospheric interface Model of the tail region of the heliospheric interface

2003-08-12

arxiv.org/abs/astro-ph/0308211v1

Astron.Lett.29:58-63,2003

Astronomy and Astrophysics

Astrophysics

first version, final version is published in Astronomy Letters vol.29 N.1, pp.58-63, 2003

Scientific paper

10.1134/1.1537379

Physical processes in the tail of the solar wind interaction region with the partially ionized local interstellar medium are investigated in a framework of the self-consistent kinetic-gas dynamic model. It is shown that the charge exchange process of the hydrogen atoms with the plasma protons results in suppression of the gas dynamic instabilities and disappearance the contact discontinuity at sufficiently (~3000 AU) large distances from the Sun. The solar wind plasma temperature decreases and, ultimately, the parameters of the plasma and hydrogen atoms approach to the corresponding parameters of the unperturbed interstellar medium at large heliocentric distances.

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