Emission line variability of RS Ophiuchi

R. K. Zamanov; M. F. Bode; N. A. Tomov; J. Porter

doi:10.1111/j.1745-3933.2005.00077.x

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arXiv · astro-ph/0506337

Emission line variability of RS Ophiuchi

R. K. Zamanov·M. F. Bode·N. A. Tomov·J. Porter

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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.

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R. K. Zamanov, M. F. Bode, N. A. Tomov, J. Porter. 2005-07-13. Emission line variability of RS Ophiuchi. https://doi.org/10.1111/j.1745-3933.2005.00077.x

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