Physics and Gasdynamics of the Heliospheric Interface |
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Authors: | Vladislav V Izmodenov |
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Institution: | (1) Faculty of Mechanicsand Mathematics, Department of Aeromechanics and Gas Dynamics,Vorob'evy Gory, Lomonosov Moscow State University, Moscow, 119899, Russia |
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Abstract: | During 30 years, a big theoretical effort to understand the physical processes in the heliospheric interface has followed
the pioneer papers by Parker (1961) and Baranov et al. (1971). The heliospheric interface is a shell formed by the solar wind interaction with the ionized component of the circumsolar
local interstellar medium (LISM). For fully ionized supersonic interstellar plasma two-shocks (the termination shock and the
bow shock) and a contact discontinuity (the heliopause) are formed in the solar wind/LISM interaction. However, LISM consists
of at least of three components additional to plasma: H-atoms, galactic cosmic rays and magnetic field. The interstellar atoms
that penetrate into the solar wind, are ionized there and form pickup ions. A part of the pickup ions is accelerated to high
energies of anomalous cosmic rays (ACRs). ACRs may modify the plasma flow upstream the termination shock and in the heliosheath.
In this short review I summarize current understanding of the physical and gasdynamical processes in the heliospheric interface,
outline unresolved problems and future perspectives.
This revised version was published online in July 2006 with corrections to the Cover Date. |
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