Anupama, G. C. ; Prabhu, T. P. (1991) H α variability in the quiescent spectrum of the recurrent nova T Coronae Borealis Monthly Notices of the Royal Astronomical Society, 253 (4). pp. 605-609. ISSN 0035-8711
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Official URL: http://mnras.oxfordjournals.org/content/253/4/605....
Related URL: http://dx.doi.org/10.1093/mnras/253.4.605
Abstract
The emission lines in the quiescent spectrum of the recurrent nova T Coronae Borealis are variable. Optical spectra recorded during the years 1985–90 show one full cycle of high and low states. After removing the slow variation, an orbital-phase-dependent variation becomes apparent in the H α line, with maxima around orbital phases 0 and 0.5. The slow variation indicates secular changes in the accretion disc possibly caused by a variable mass transfer rate. Orbital variations can be caused either by geometrical effects or a phase-modulated mass transfer rate. More detailed monitoring is needed to model the system.
Item Type: | Article |
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Source: | Copyright of this article belongs to Oxford University Press. |
ID Code: | 100451 |
Deposited On: | 10 Dec 2016 13:01 |
Last Modified: | 10 Dec 2016 13:01 |
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