Please use this identifier to cite or link to this item:
Full metadata record
DC FieldValueLanguage
dc.contributor.authorAnupama, G. C-
dc.contributor.authorMikołajewska, J-
dc.identifier.citationAstronomy and Astrophysics, Vol. 344, No. 1, pp. 177 - 187en
dc.identifier.issn0004 - 6361-
dc.description.abstractSpectroscopic and photometric behaviour of the class of recurrent novae with giant secondaries (T Coronae Borealis, RS Ophiuchi, V3890 Sagittarii and V745 Scorpii) at quiescence are presented in this study. The hot component in these systems is variable, with the variability manifesting as variability in the ultraviolet luminosity, the ultraviolet and optical emission line fluxes and in the UBV/visual magnitudes. The variations are uncorrelated with the binary orbital motion. The observed ultraviolet+optical spectral characteristics of the hot component in these systems can be explained by a white dwarf+accretion disc embedded in an envelope of wind from the M giant secondary. We suggest that the observed variations are a result of (a) fluctuations in the mass accretion rate; (b) changes in the column density of the absorbing wind envelope, which is optically thick.en
dc.format.extent464632 bytes-
dc.publisherEuropean Southern Observatoryen
dc.subjectT CRBen
dc.subjectRS OPHen
dc.subjectV745 SCOen
dc.subjectV3890 SGRen
dc.titleRecurrent novae at quiescence: systems with giant secondariesen
Appears in Collections:IIAP Publications

Files in This Item:
File Description SizeFormat 
Recurrent novae at quiescence453.74 kBAdobe PDFView/Open

Items in DSpace are protected by copyright, with all rights reserved, unless otherwise indicated.