Kinetic modeling of the H atoms in the heliospheric interface: solar cycle effects

Details Kinetic modeling of the H atoms in the heliospheric interface: solar cycle effects Kinetic modeling of the H atoms in the heliospheric interface: solar cycle effects

Sep 2004

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004aipc..719...47i&link_type=abstract

PHYSICS OF THE OUTER HELIOSPHERE. AIP Conference Proceedings, Volume 719, pp. 47-52 (2004).

Physics

6

Particle Emission, Solar Wind, Solar Wind Plasma, Sources Of Solar Wind, Planetary Bow Shocks, Interplanetary Shocks

Scientific paper

In this paper we present results of a new time-dependent kinetic model of the H atom penetration through the solar wind - interstellar medium interaction region. The 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 the 11 year solar cycle variations of the solar wind. The termination shock location varies within +/-7 AU, the heliopause variation is ~2 AU, and the bow shock variation is negligible. At large heliocentric distances, the solar cycle induces 10-12 % of fluctuations in the number density of both primary and secondary interstellar H atoms and atoms created in the inner heliosheath. Closer to the Sun the variation increases up to 30-35 % at 5 AU due to the 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 a major importance for the interpretation of H atom observations inside the heliosphere.

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