Seismology of the Accreting White Dwarf in GW Lib

Details Seismology of the Accreting White Dwarf in GW Lib Seismology of the Accreting White Dwarf in GW Lib

2004-05-07

arxiv.org/abs/astro-ph/0405132v1

Astrophys.J. 608 (2004) L105-L108

Astronomy and Astrophysics

Astrophysics

4 pages, 3 figures; uses emulateapj; Accepted by the Astrophysical Journal Letters

Scientific paper

10.1086/422411

We present a first analysis of the g-mode oscillation spectrum for the white dwarf (WD) primary of GW Lib, a faint cataclysmic variable (CV). Stable periodicities have been observed from this WD for a number of years, but their interpretation as stellar pulsations has been hampered by a lack of theoretical models appropriate to an accreting WD. Using the results of Townsley and Bildsten, we construct accreting models for the observed effective temperature and approximate mass of the WD in GW Lib. We compute g-mode frequencies for a range of accreted layer masses, Macc, and long term accretion rates, . If we assume that the observed oscillations are from l=1 g-modes, then the observed periods are matched when M ~= 1.02 Msun, Macc ~= 0.31 x 10^-4 Msun and ~= 7.3 x 10^-11 Msun/yr. Much more sensitive observations are needed to discover more modes, after which we will be able to more accurately measure these parameters and constrain or measure the WD's rotation rate.

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