Time-resolved spectroscopy of the pulsating CV GW Lib
van Spaandonk, Lieke, Steeghs, D., Marsh, T. R. and Torres, M. A. P.. (2010) Time-resolved spectroscopy of the pulsating CV GW Lib. Monthly Notices of the Royal Astronomical Society, Vol.401 (No.3). pp. 1857-1868. ISSN 0035-8711
WRAP_Steeghs_CV_GW_Lib_0909.3991v1.pdf - Accepted Version
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Official URL: http://dx.doi.org/10.1111/j.1365-2966.2009.15762.x
We present time-resolved optical spectroscopy of the dwarf nova GW Librae during its rare 2007 April superoutburst and compare these with quiescent epochs. The data provide the first opportunity to track the evolution of the principal spectral features. In the early stages of the outburst, the optically thick disc dominates the optical and the line components show clear orbital radial velocity excursions. In the course of several weeks, optically thin regions become more prominent as strong emission lines replace the broad disc absorption.
Post-outburst spectroscopy covering the I band illustrates the advantages of Ca II relative to the commonly used Balmer lines when attempting to constrain binary parameters. Due to the lower ionization energy combined with smaller thermal and shear broadening of these lines, a sharp emission component is seen to be moving in between the accretion disc peaks in the Ca II line. No such component is visible in the Balmer lines. We interpret this as an emission component originating on the hitherto unseen mass donor star. This emission component has a mean velocity of similar to -15 +/- 5 km s(-1) which is associated with the systemic velocity., and a velocity semi-amplitude of K-em = 82.2 +/- 4.9 km s(-1). Doppler tomography reveals an asymmetric accretion disc, with the S-wave mapping to a sharp spot in the tomogram with a velocity consistent to what is obtained with line profile fitting. A centre of symmetry analysis of the disc component suggests a very small value for the WD orbital velocity K-1 as is also inferred from double Gaussian fits to the spectral lines.
While our conservative dynamical limits place a hard upper limit on the binary mass ratio of q < 0.23, we favour a significantly lower value near q similar to 0.06. Pulsation modelling suggests a white dwarf mass similar to 1 M-circle dot. This, paired with a low-mass donor, near the empirical sequence of an evolved cataclysmic variable close to the period bounce, appears to be consistent with all the observational constraints to date.
|Item Type:||Journal Article|
|Subjects:||Q Science > QB Astronomy|
|Divisions:||Faculty of Science > Physics|
|Library of Congress Subject Headings (LCSH):||Dwarf novae|
|Journal or Publication Title:||Monthly Notices of the Royal Astronomical Society|
|Official Date:||21 January 2010|
|Number of Pages:||12|
|Page Range:||pp. 1857-1868|
|Access rights to Published version:||Restricted or Subscription Access|
|Funder:||Science and Technology Facilities Council (Great Britain) (STFC)|
Araujo-Betancor S., G¨ansicke B.T., Hagen H.-J. et al.,
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