Rate of change of the pulsation periods in the PG 1159 star PG 0122+200

Details Rate of change of the pulsation periods in the PG 1159 star PG 0122+200 Rate of change of the pulsation periods in the PG 1159 star PG 0122+200

Oct 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008iaus..252..157v&link_type=abstract

The Art of Modeling Stars in the 21st Century, Proceedings of the International Astronomical Union, IAU Symposium, Volume 252, p

Other

Neutrinos, Stars:Evolution, Stars: Individual (Pg 0122+200), Stars: Oscillations, Stars: White Dwarfs

Scientific paper

The pre-white dwarf pulsators of PG 1159 type, or GW Virginis variable stars, are in a phase of rapid evolution towards the white dwarf cooling sequence. The rate of change of their nonradial g-mode frequencies can be measured on a reasonably short time scale. From a theoretical point of view, it was expected that one could derive the rate of cooling of the stellar core from such measurements. At the cool end of the GW Virginis instability strip, it is predicted that the neutrinos flux dominates the cooling. PG 0122+200 which defines the red edge of the instability strip is in principle a good candidate to check this prediction. It has been followed-up through multisite photometric campaigns for about fifteen years. We report here the first determination of the rate of change of its 7 largest amplitude frequencies. We find that the amplitudes of the frequency variations are one to two orders of magnitude larger than predicted by theoretical models based on the assumption that these variations are uniquely caused by cooling. The time scales of the variations are much shorter than the ones expected from a neutrino dominated core cooling. These results point to the existence of other mechanisms responsible for the frequency variability. We discuss the role of nonlinearities as one possible mechanism.

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