Seismology of Accreting White Dwarfs：（地震学合生的白矮星）.pdfVIP

Seismology of Accreting White Dwarfs 1 2 1,2 Phil Arras , Dean Townsley , Lars Bildsten 1Kavli Institute for Theoretical Physics, Kohn Hall, University of 4 California, Santa Barbara, CA 93106 0 2 Department of Physics, Broida Hall, University of California, Santa 0 Barbara, CA 93106 2 t c Abstract. Pulsation modes have recently been observed in a handful of O white dwarf (WD) primaries of cataclysmic variables, allowing an interesting new probe into the structure of accreting WD’s. We briefly discuss the seismology 2 of these objects, how stellar properties may be inferred from the observed mode 1 frequencies, and mode driving mechanisms. For one pulsator, GW Lib, we have shown that a WD mass M = 1.05 M⊙ and accreted envelope mass Menv = 1 −4 v 0.4 × 10 M⊙ give the best match to the observed pulsation periods. A first 3 exploration of mode driving favors Teff = 14000K and a massive WD, but more 1 work is necessary. 3 0 1 4 0 1. Introduction / h Pulsation modes have been observed in isolated white dwarfs for several decades. p - Since the observed mode periods are sensitive to the WD structure, an industry o has emerged to estimate parameters such as WD mass, light element envelope r t mass, and rotation rate from observed the mode periods (for a review, see e.g. s a Bradl