Seismology of the accreting white dwarf in GW librae

We present a first analysis of the g-mode oscillation spectrum for the white dwarf (WD) primary of GW Lib, a faint cataclysmic variable. 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 & 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, M-acc, and long-term accretion rates, <M>. If we assume that the observed oscillations are from l = 1 g-modes, then the observed periods are matched when M approximate to 1.02 M, M-acc approximate to 0.31 x 10(-4) M-circle dot, and <M> approximate to 7.3 x 10(-11) M-circle dot yr(-1). 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.