Emission line variability of RS Ophiuchi

Abstract

We report that the H_alpha emission line of RS Oph was strongly variable during our 2004 observations on a time scale of 1 month. The line consisted of both a double peaked central narrow component (FWHM ~ 220 km/s) and a strongly variable broad one (FWHM ~ 2000 km/s). The base of the H_alpha line was very broad with FWZI 4600 km/s on all spectra from 1986 to 2004. The variability of the broad component extends from -2000 to +2000 km/s. Most probably this is due to either blobs ejected from the white dwarf (with a typical blob mass estimated to be ~10^{-10} M_solar or a variable accretion disk wind. We also detected variability of the HeII4686 line on a time scale shorter than 1 day. The possible origin is discussed.

accepted in MNRAS (letters)

References in corpus (6)

• Recurrent novae as a progenitor system of Type Ia supernovae. I. RS Ophiuchi subclass --- Systems with a red giant companion
• H-alpha variability of the recurrent nova T Coronae Borealis
• High-Speed Optical Spectroscopy of a Cataclysmic Variable Wind: BZ Camelopardalis
• The spectroscopic orbits and the geometrical configuration of the symbiotic binary AR Pavonis
• A theoretical light-curve model for the 1985 outburst of RS Ophiuchi
• Rapid H-alpha variability in T Coronae Borealis

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• AG Pegasi - now a classical symbiotic star in outburst?
• Design and Development of Mt. Abu Faint Object Spectrograph and Camera -- Pathfinder (MFOSC-P) for PRL 1.2m Mt. Abu Telescope
• High-resolution optical spectroscopy of RS Ophiuchi during 2008 -- 2009
• Multiwavelength modelling the SED of supersoft X-ray sources III. RS Ophiuchi: The supersoft X-ray phase and beyond
• Simultaneous UBVRI observations of the cataclysmic variable AE Aquarii: temperature and mass of fireballs