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X-ray emission from cataclysmic variables with accretion disks. I - Hard X-rays. II - EUV/soft X-ray radiationTheoretical models explaining the hard-X-ray, soft-X-ray, and EUV emission of accretion-disk cataclysmic variables in terms of the disk boundary layer (DBL) are developed on the basis of a survey of the published observational data. The data are compared with model predictions in graphs for systems with high or low (greater than or less than 10-Pg/s) accretion rates. Good agreement is obtained both at low accretion rates, where an optically thin rarefied hot (Te = 10 to the 8th K) DBL radiates most of its energy as hard X-rays, and at high accretion rates, where an optically thick 100,000-K DBL radiates most of its energy in the EUV and as soft X-rays. Detailed analysis of the old nova V603 Aql suggests that previous models predicting more detections of soft-X-ray/EUV emissions from thick-DBL objects (Ferland et al., 1982) used inappropriate dwarf masses, interstellar column densities, or classical-nova space densities.
Document ID
19850054650
Acquisition Source
Legacy CDMS
Document Type
Reprint (Version printed in journal)
External Source(s)
Authors
Patterson, J.
(Columbia University New York, NY, United States)
Raymond, J. C.
(Harvard-Smithsonian Center for Astrophysics Cambridge, MA, United States)
Date Acquired
August 12, 2013
Publication Date
May 15, 1985
Publication Information
Publication: Astrophysical Journal, Part 1
Volume: 292
ISSN: 0004-637X
Subject Category
Astrophysics
Accession Number
85A36801
Funding Number(s)
CONTRACT_GRANT: NAGW-117
CONTRACT_GRANT: NAG8-497
CONTRACT_GRANT: NAS8-30453
Distribution Limits
Public
Copyright
Other

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