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Cosmic-ray-modified supernova remnant shocksThe evolution of cosmic-ray-modified SNRs during the early Sedov phase is investigated using the time-dependent, two-fluid model for diffusive shock acceleration. Consideration is given to the sensitivity of net acceleration efficiency to model assumptions regarding density structure of the external medium as well as time dependence in the diffusion coefficient and the cosmic-ray adiabatic index. Of the model assumptions explored, the greatest sensitivity was found to time variations in the specific heat ratio to cosmic rays. It was found that if tau is greater than or approximately equal to few times 100, dynamically significant cosmic-ray pressures are produced early in the Sedov inefficient cosmic-ray accelerators. For the SNR models under consideration, the total energy channeled into the cosmic rays can be of order 10 percent of the initial blast energy for both the uniform density and inverse-square density interstellar medium models.
Document ID
19920071743
Acquisition Source
Legacy CDMS
Document Type
Reprint (Version printed in journal)
External Source(s)
Authors
Jones, T. W.
(Minnesota, University Minneapolis, United States)
Kang, Hyesung
(Minnesota, University Minneapolis; Princeton University Observatory, NJ, United States)
Date Acquired
August 15, 2013
Publication Date
September 10, 1992
Publication Information
Publication: Astrophysical Journal, Part 1
Volume: 396
Issue: 2 Se
ISSN: 0004-637X
Subject Category
Astrophysics
Accession Number
92A54367
Funding Number(s)
CONTRACT_GRANT: NAGW-2548
CONTRACT_GRANT: NSF AST-91-00486
CONTRACT_GRANT: NSF AST-87-20285
Distribution Limits
Public
Copyright
Other

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