Modification of the local interstellar gas properties in the heliospheric interface

Details Modification of the local interstellar gas properties in the heliospheric interface Modification of the local interstellar gas properties in the heliospheric interface

Jun 1983

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1983a%26a...122..181r&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 122, no. 1-2, June 1983, p. 181-192.

Astronomy and Astrophysics

Astrophysics

111

Heliosphere, Interplanetary Space, Interstellar Gas, Luminescence, Boltzmann Transport Equation, Hydrogen Atoms, Integral Equations, Kinetic Theory, Resonance, Solar System

Scientific paper

Conventional methods to determine the local interstellar matter (LISM) parameters on the basis of theoretical interpretations of interplanetary resonance luminescence patterns have been questioned in recent years because of physically incompatible results. It appears that these incompatibilities can be resolved by a consideration of the perturbing effects of the heliospheric interface on the interstellar gases. In this paper kinetic theory concepts are used for the quantitative description of these effects. It is shown that hydrogen streaming through the interface suffers temperature changes of about 1500K and bulk velocity changes of about 1 km s-1. The main effect of the interface, however, consists of a density decrease by 40-60%, irrespective of the type of interface model that is considered. The LISM ionization degree turns out to be lower than 20%, the heliocentric distance to the heliopause substantially exceeds 100 AU, and the deduced LISM abundance ratio between helium and hydrogen is consistent with the classical values.

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