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X-ray Novae and Related SystemsAccretion disk thermal instability models have been successful in accounting for the basic observations of dwarf novae and the steady behavior of nova-like systems. Models for the dwarf-nova like variability of the old nova and intermediate polar GK Per give good agreement with the burst amplitude, profile and recurrence time in the optical and UV. A month-long 'precursor plateau' in the UV is predicted for the expected 1992 outburst prior to the rise to maximum in the optical and UV. The models for the time scales of the outbursts and corresponding UV spectra at maximum are consistent with the inner edge of the accretion disk being essentially constant between quiescence and outburst and a factor of four larger than the co-rotation radius. These conclusions represent a challenge to the standard theory of magnetic accretion. Disk instability models have also given a good representation of the soft X-ray and optical outbursts of the X-ray novae A0620-00 and GS2000+25. Formation of coronae above the disk, heated by magneto-acoustic flux from the disk, may account for the temporal and spectral properties of the hard X-ray and gamma ray emission of related sources such as Cyg X-1, GS 2023+33 (V404 Cyg), IE 1740.7-2942 (the 'Galactic Center' Einstein Source), and GS 1124-683 (Nova Muscae).
Document ID
19970020422
Acquisition Source
Headquarters
Document Type
Reprint (Version printed in journal)
Authors
Wheeler, J. Craig
(Texas Univ. Austin, TX United States)
Kim, Soonwook
(Texas Univ. Austin, TX United States)
Mineshige, Shin
(Ibaraki Univ. Mito, Japan)
Date Acquired
August 17, 2013
Publication Date
January 1, 1992
Publication Information
Publication: Evolutionary Processes in Interacting Binary Stars
Publisher: IAU
Subject Category
Astronomy
Report/Patent Number
NAS 1.26:203797
NASA-CR-203797
Accession Number
97N71970
Funding Number(s)
CONTRACT_GRANT: NSF-8915754
CONTRACT_GRANT: NAGw-1807
Distribution Limits
Public
Copyright
Public Use Permitted.
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