Physics
Scientific paper
May 2000
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2000ohbp.conf...91s&link_type=abstract
"In: The outer heliosphere: beyond the planets. Based on the spring school "Die äußere Heliosphäre - Jenseits der Planeten, in B
Physics
1
Interplanetary Gas
Scientific paper
The neutral hydrogen, embedded in the partially ionized local interstellar medium, can enter deeply into the heliosphere with the interstellar wind flow. While entering into the heliosphere it suffers from intense charge-exchange interactions with the solar wind protons. This charge-exchange leads to a fractional depletion of the interstellar hydrogen atoms inside the heliosphere and modulates their velocity and temperature distribution. The resulting thermodynamical conditions of the interstellar hydrogen inside the heliosphere are described by two kinetic density models. The first model by Wu & Judge specially takes into account the influence on hydrogen due to solar photo ionization and solar gravitation and leads to appropriate results in the solar vicinity. The second model by Osterbart & Fahr takes into account the plasma interaction effects near the solar wind shock region and near the heliopause. Hence, this model gives more realistic results for the hydrogen properties far away from the Sun. Besides these theoretical modelings of the interplanetary hydrogen, measurements of the interplanetary hydrogen HI-Lyman-Alpha resonance glow were performed and attempts have been made to deduce the relevant thermodynamical parameter of the neutral interstellar hydrogen by analyzing these glow data. Two radiation transport models will be discussed which are used to analyze the interplanetary hydrogen HI-Lyman-Alpha resonance glow data. First, the "optically thin" approximation which is used very often in the literature because of its simple numerical handling. Unfortunately, this model has a very limited region of validity. The second radiation transport model by Scherer & Fahr introduces the exact redistribution function which takes into account the local thermodynamical conditions of the scattering agent, like density, bulk velocity and temperature of the neutral interplanetary hydrogen. Also it takes into account the actually observed solar HI-Lyman-Alpha emission profile. Therefore it is a significant improvement with respect to the "optically thin" approximation but causes much more numerical efforts.
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