X-ray emission from cataclysmic variables with accretion disks. I - Hard X-rays. II - EUV/soft X-ray radiation
In: Astrophysical Journal, Part 1, Jg. 292 (1985-05-15)
Online
report
Theoretical 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.
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X-ray emission from cataclysmic variables with accretion disks. I - Hard X-rays. II - EUV/soft X-ray radiation
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Autor/in / Beteiligte Person: | Patterson, J ; Raymond, J. C |
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Zeitschrift: | Astrophysical Journal, Part 1, Jg. 292 (1985-05-15) |
Veröffentlichung: | United States: NASA Center for Aerospace Information (CASI), 1985 |
Medientyp: | report |
ISSN: | 0004-637X (print) |
DOI: | 10.1086/163187 |
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