Asteroseismological measurements on PG 1159-035, the prototype of the GW Vir variable stars

Abstract

An asteroseismological study of PG 1159-035, the prototype of the GW Vir variable stars, has been performed on the basis of detailed and full PG1159 evolutionary models presented by Miller Bertolami & Althaus (2006). We carried out extensive computations of adiabatic g-mode pulsation periods on PG1159 evolutionary models with stellar masses spanning the range 0.530 to 0.741 Mo. We derive a stellar mass in the range 0.56-0.59 Mo from the period-spacing data alone. We also find, on the basis of a period-fit procedure, a seismic model representative of PG 1159-035 that reproduces the observed period pattern with an average of the period differences of 0.64-1.03 s, consistent with the expected model uncertainties. The results of the period-fit analysis carried out in this work suggest that the surface gravity of PG 1159-035 would be 1 sigma larger than the spectroscopically inferred gravity. For our best-fit model of PG 1159-035, all of the pulsation modes are characterized by positive rates of period changes, at odds with the measurements by Costa & Kepler (2007).

14 pages, 11 figures, 5 tables. To be published in Astronomy & Astrophysics

References in corpus (7)

• Asteroseismic inferences on GW Vir variable stars in the frame of new PG 1159 evolutionary models
• New nonadiabatic pulsation computations on full PG1159 evolutionary models: the theoretical GW Vir instability strip revisited
• The pulsation modes of the pre-white dwarf PG 1159-035
• Asteroseismological constraints on the pulsating planetary nebula nucleus (PG1159-type) RX J2117.1+3412
• The born again (VLTP) scenario revisited: The mass of the remnants and implications for V4334 Sgr
• Asteroseismological constraints on the coolest GW Vir variable star (PG 1159-type)PG 0122+200
• On the robustness of H-deficient post-AGB tracks

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