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Record 9 of 528
The spectral evolution of dwarf nova outbursts
External Online Source: doi:10.1086/165545
Author and Affiliation:
Cannizzo, John K.(Harvard-Smithsonian Center for Astrophysics, Cambridge, MA, United States)
Kenyon, Scott J.(Harvard-Smithsonian Center for Astrophysics, Cambridge, MA, United States)
Abstract: The disk instability model for dwarf nova eruptions is investigated by computing the spectral development of the accretion disk through a complete limit cycle. Observed stellar spectra are used to model the radiation emitted by optically thick annuli within the disc. The general findings agree with those of Smak (1984) and Pringle et al. (1986). It is suggested that the 'dwarf nova oscillations' might be a source of information concerning the evolution of the inner disk and that detailed observations of this phenomenon can be used to test various outburst mechanisms.
Publication Date: Sep 01, 1987
Document ID:
19880023100
(Acquired Nov 28, 1995)
Accession Number: 88A10327
Subject Category: ASTROPHYSICS
Document Type: Journal Article
Publication Information: Astrophysical Journal, Part 1 (ISSN 0004-637X); 320; 319-332
Publisher Information: United States
Contract/Grant/Task Num: NSERC-5-37687; NGR-22-007-272
Financial Sponsor: NASA; United States
Organization Source: Harvard-Smithsonian Center for Astrophysics; Cambridge, MA, United States
Description: 14p; In English
Distribution Limits: Unclassified; Publicly available; Unlimited
Rights: Copyright
NASA Terms: DWARF NOVAE; STELLAR EVOLUTION; STELLAR MODELS; STELLAR OSCILLATIONS; STELLAR SPECTRA; STELLAR STRUCTURE; BINARY STARS; OPTICAL THICKNESS; STELLAR MASS ACCRETION; ULTRAVIOLET SPECTRA; WHITE DWARF STARS
Imprint And Other Notes: Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 320, Sept. 1, 1987, p. 319-332.
Availability Source: Other Sources
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