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 ≈ 1.02 solar mass, M_(acc) ≈ 0.31 x 10~(-4) solar mass, and < M > ≈ 7.3 x 10~(-11) solar mass 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.
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机译：我们目前对GW Lib的白矮星（WD）的g模式振荡光谱进行了首次分析，这是一个微弱的灾难性变量。多年来已经从该WD观察到了稳定的周期，但是由于缺乏适合于吸积WD的理论模型，它们对恒星脉动的解释受到阻碍。使用Townsley＆Bildsten的结果，我们为观测到的有效温度和GW Lib中WD的近似质量构建了吸积模型。我们为一定范围的堆积层质量M_（acc）和长期堆积率计算g模式频率。如果我们假设观测到的振荡来自l = 1 g-modes，那么当M≈1.02太阳质量，M_（acc）≈0.31 x 10〜（-4）太阳质量且≈ 7.3 x 10〜（-11）太阳质量yr〜（-1）。需要更多敏感的观测结果以发现更多模式，之后我们将能够更准确地测量这些参数，并约束或测量WD的旋转速率。
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