  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).
