H-alpha variability in the quiescent spectrum of the recurrent nova T Coronae Borealis

dc.contributor.author	Anupama, G. C
dc.contributor.author	Prabhu, T. P
dc.date.accessioned	2008-07-02T11:00:28Z
dc.date.available	2008-07-02T11:00:28Z
dc.date.issued	1991-12
dc.identifier.citation	MNRAS, Vol. 253, No.4, pp. 605 - 609	en
dc.identifier.issn	0035-8711
dc.identifier.uri	http://hdl.handle.net/2248/2575
dc.description.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-alpha line, with maxima around orbital phases 0 and 0.5. The slow variation indicates secular changes in the accretion disk 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.	en
dc.format.extent	955569 bytes
dc.format.mimetype	application/pdf
dc.language.iso	en	en
dc.publisher	Blackwell Publishing	en
dc.relation.uri	http://adsabs.harvard.edu/abs/1991MNRAS.253..605A	en
dc.subject	H alpha line	en
dc.subject	Novae	en
dc.subject	Stellar spectra	en
dc.subject	Variable stars	en
dc.subject	Emission spectra	en
dc.subject	Spectral line width	en
dc.subject	Variability	en
dc.subject	Visible spectrum	en
dc.title	H-alpha variability in the quiescent spectrum of the recurrent nova T Coronae Borealis	en
dc.type	Article	en