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Application of cosmic-ray shock theories to the Cygnus Loop - An alternative modelSteady state cosmic-ray shock models are investigated here in the light of observations of the Cygnus Loop supernova remnant. The predicted downstream temperature is derived for each model. The Cygnus Loop data and the application of the models to them, including wave dissipation, are presented. Heating rate and ionization fraction structures are provided along with an estimate of the cosmic-ray diffusion coefficient. It is found that the model of Voelk, Drury, and McKenzie (1984), in which the plasma waves are generated by the streaming instability of the cosmic rays and are dissipated into the gas, can be made consistent with some observed characteristics of the Cygnus Loop shocks. The model is used to deduce upstream densities and shock velocities and, compared to the usual pure gas shock interpretation, it is found that lower densities and approximately three times higher velocities are required.
Document ID
19890023048
Acquisition Source
Legacy CDMS
Document Type
Reprint (Version printed in journal)
External Source(s)
Authors
Boulares, Ahmed
(Wisconsin Univ. Madison, WI, United States)
Cox, Donald P.
(Wisconsin, University Madison, United States)
Date Acquired
August 13, 2013
Publication Date
October 1, 1988
Publication Information
Publication: Astrophysical Journal, Part 1
Volume: 333
ISSN: 0004-637X
Subject Category
Astrophysics
Accession Number
89A10419
Funding Number(s)
CONTRACT_GRANT: NSF AST-86-43609
CONTRACT_GRANT: NAG5-629
Distribution Limits
Public
Copyright
Other

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