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

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

Dec 1991

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991mnras.253..605a&link_type=abstract

Monthly Notices of the Royal Astronomical Society (ISSN 0035-8711), vol. 253, Dec. 15, 1991, p. 605-609.

Astronomy and Astrophysics

Astronomy

8

H Alpha Line, Novae, Stellar Spectra, Variable Stars, Emission Spectra, Spectral Line Width, Variability, Visible Spectrum

Scientific paper

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.

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