Model of the tail region of the heliospheric interface
arXiv:astro-ph/0308211 · doi:10.1134/1.1537379
Abstract
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.
arXiv commentfirst version, final version is published in Astronomy Letters vol.29 N.1, pp.58-63, 2003
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