The Stellar Seismology of the Hot White Dwarf Star PG:1159-035

A simple empirical model of the observed period spectrum of the hot white dwarf star PG 1159-035 yields two statistically significant mean period intervals of 21.0±0.3 or 8.8±0.1 s. The author also evaluates the period interval for models of hot white dwarfs that are representative of PG 1159 stars. The observed intervals correspond very closely to those derived from the theoretical models. This analysis indicates that the mass of PG 1159-035 is 0.60 M_sun; and that it is either a dipole (l = 1) or l = 3 pulsator (or both!), pulsating in high radial overtone g-modes.