Solar cycle influence on the interaction of the solar wind with Local Interstellar Cloud

被引:90
作者
Izmodenov, V [1 ]
Malama, Y
Ruderman, MS
机构
[1] Moscow MV Lomonosov State Univ, Dept Aeromech & Gas Dynam, Fac Mech & Math, Moscow 119899, Russia
[2] Inst Mech, Moscow 119899, Russia
[3] Russian Acad Sci, Inst Problems Mech, Moscow 117526, Russia
[4] Univ Sheffield, Dept Appl Math, Sheffield S3 7RH, S Yorkshire, England
关键词
Sun : solar wind; interplanetary medium; ISM : atoms; Sun : activity; hydrodynamics;
D O I
10.1051/0004-6361:20041348
中图分类号
P1 [天文学];
学科分类号
0704 ;
摘要
We present results of a new time-dependent kinetic model of the H atom penetration through the solar wind interstellar medium interaction region. A kinetic 6D (time, two dimensions in space, and three dimensions in velocity-space) equation for interstellar H atoms was solved self-consistently with time-dependent Euler equations for the solar wind and interstellar charged components. We study the response of the interaction region to 11-year solar cycle variations of the solar wind dynamic pressure. It is shown that the termination shock location varies within +/-7 AU, the heliopause variation is similar to4 AU, and the bow shock variation is negligible. At large heliocentric distances, the solar cycle induces 10-12% fluctuations in the number density of both primary and secondary interstellar H atoms and atoms created in the inner heliosheath. We underline the kinetic behavior of the fluctuations of the H atom populations. Closer to the Sun the fluctuations increase up to 30-35% at 5 AU due to solar cycle variation of the charge exchange rate. Solar cycle variations of interstellar H atoms in the heliospheric interface and within the heliosphere may have major importance for the interpretation of H atom observations inside the heliosphere.
引用
收藏
页码:1069 / U17
页数:18
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