Astronomy and Astrophysics – Astronomy
Scientific paper
Aug 1983
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1983mnras.204..537b&link_type=abstract
Monthly Notices of the Royal Astronomical Society (ISSN 0035-8711), vol. 204, Aug. 1983, p. 537-556. Research supported by the U
Astronomy and Astrophysics
Astronomy
48
Stellar Envelopes, Stellar Oscillations, White Dwarf Stars, Hydrogen, Light Curve, Stellar Temperature
Scientific paper
The linear non-adiabatic calculations of Dolez and Vauclair show that for the g-modes associated with a given value of l there is a critical frequency for each model. Only modes which vary on a shorter time-scale are vibrationally unstable. In this paper it is shown that in these modes the perturbation to the pressure varies little through the hydrogen driving zone and, on this basis, flux variations of finite amplitude have been computed. The results of these calculations explain many of the characteristic features of the ZZ Cetis. In particular it is shown that for a given star there is a restricted interval in frequency where pulsations of large amplitude can be observed. As the effective temperature decreases this interval moves into the range where the frequency is smaller than the critical value for all the g-modes. This point coincides with the upper limit in the observed period range of the ZZ Cetis and explains the observational red edge.
No associations
LandOfFree
The pulsations of ZZ Ceti stars does not yet have a rating. At this time, there are no reviews or comments for this scientific paper.
If you have personal experience with The pulsations of ZZ Ceti stars, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and The pulsations of ZZ Ceti stars will most certainly appreciate the feedback.
Profile ID: LFWR-SCP-O-748656