Astronomy and Astrophysics – Astrophysics
Scientific paper
Jun 1987
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987a%26a...180..201b&link_type=abstract
Astronomy and Astrophysics (ISSN 0004-6361), vol. 180, no. 1-2, June 1987, p. 201-206.
Astronomy and Astrophysics
Astrophysics
39
Heliosphere, Interstellar Matter, Plasma Interactions, Plasmapause, Stellar Models, Monte Carlo Method, Neutral Gases, Solar System
Scientific paper
Monte Carlo simulation of heliospheric penetration of the neutral interstellar atoms was performed for the Baranov-like heliopause model, following trajectories of individual H, He, or O atoms through the whole heliospheric plasma interface system. The results show that the fraction of gas which penetrates the inner heliosphere significantly differs from the original one of the local ISM (LISM). For initial LISM proton and hydrogen densities of 0.04 and 0.07/cu cm, respectively, bulk velocity of 28 km/s, and temperature of 9100 K the following two populations of cool inner heliospheric H are obtained: a primary one with bulk velocity Vz = 30 km/s, density = 0.026/cu cm, temperature = 9000 K, and a secondary one with Vz = 16 km/s, density = 0.019/cu cm, and temperatures of about 10,000 K and 13,000 K parallel and perpendicular to the flow, respectively. The fraction of LISM neutral oxygen penetrating the heliosphere depends much more strongly on LISM parameters and varies from 0.1 to 0.7. Helium passes through the whole interface almost unaffected.
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