Open AccessEmission line variability of RS Ophiuchi ★
Author(s) -
Zamanov R. K.,
Bode M. F.,
Tomov N. A.,
Porter J. M.
Publication year - 2005
Publication title -
monthly notices of the royal astronomical society: letters
Language(s) - English
Resource type - Journals
SCImago Journal Rank - 2.067
H-Index - 122
eISSN - 1745-3933
pISSN - 1745-3925
DOI - 10.1111/j.1745-3933.2005.00077.x
Subject(s) - astrophysics , full width at half maximum , physics , emission spectrum , white dwarf , line (geometry) , spectral line , cataclysmic variable star , variable star , equivalent width , astronomy , line width , stars , geometry , optics , mathematics
We report that the Hα emission line of RS Oph was strongly variable during our 2004 observations on a time‐scale of one month. The line consisted of both a double‐peaked central narrow component [full width at half‐maximum (FWHM) ∼ 220 km s −1 ] and a strongly variable broad one (FWHM > 2000 km s −1 ). The base of the Hα line was very broad, with full width at zero intensity ≈ 4600 km s −1 on all spectra from 1986 to 2004. The variability of the broad component extends from −2000 to +2000 km s −1 . Most probably this is due either to blobs ejected from the white dwarf (with a typical blob mass estimated to be ∼10 −10 M ⊙ ) or to a variable accretion disc wind. We also detected variability of the He ii λ4686 line on a time‐scale shorter than 1 d. The possible origin is discussed.