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Galactic cosmic-ray mediation of a spherical solar wind flow. 1: The steady state cold gas hydrodynamical approximationRealistic models of the outer heliosphere should consider that the interstellar cosmic-ray pressure becomes comparable to pressures in the solar wind at distances more than 100 AU from the Sun. The cosmic-ray pressure dynamically affects solar wind flow through deceleration. This effect, which occurs over a scale length of the order of the effective diffusion length at large radial distances, has important implications for cosmic-ray modulation and acceleration. As a first step toward solution of this nonlinear problem, a steady state numerical model was developed for a relatively cold spherical solar wind flow which encounters the confining isotropic pressure of the surrounding Galactic medium. This pressure is assumed to be dominated by energetic particles (Galactic cosmic rays). The system of equations, which are solved self-consistently, includes the relevant hydrodynamical equations for the solar wind flow and the spherical cosmic-ray transport equation. To avoid the closure parameter problem of the two-fluid model, the latter equation is solved for the energy-dependent cosmic-ray distribution function.
Document ID
19950048265
Acquisition Source
Legacy CDMS
Document Type
Reprint (Version printed in journal)
External Source(s)
Authors
Le Roux, J. A.
(Univ. of Maryland, College Park, MD United States)
Ptuskin, V. S.
(Russian Academy of Sciences Troitsk, Russia)
Date Acquired
August 16, 2013
Publication Date
January 1, 1995
Publication Information
Publication: Astrophysical Journal, Part 1
Volume: 438
Issue: 1
ISSN: 0004-637X
Subject Category
Space Radiation
Accession Number
95A79864
Funding Number(s)
CONTRACT_GRANT: NAG5-1299
CONTRACT_GRANT: NAGW-2504
CONTRACT_GRANT: NAG2-627
Distribution Limits
Public
Copyright
Other

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