Theoretical radial pulsation analyses of DA white dwarfs

Details Theoretical radial pulsation analyses of DA white dwarfs Theoretical radial pulsation analyses of DA white dwarfs

Jun 1983

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1983apj...269..645s&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 269, June 15, 1983, p. 645-656. Research supported by the U.S. Department o

Astronomy and Astrophysics

Astrophysics

10

Stellar Envelopes, Stellar Oscillations, White Dwarf Stars, Helium, Hydrogen, Nonadiabatic Theory, Vibration Mode

Scientific paper

A linear, nonadiabatic, radial pulsation analysis of DA white dwarfs has been conducted, taking into account the range of effective temperatures from 7,000 to 12,500 K. The considered 0.6 solar mass, 0.013 solar radius model envelopes consist of layers of pure hydrogen overlying layers of pure helium and pure carbon. It is found that these envelopes are unstable to radial pulsations with periods less than 1.0 s and that the cause of the instability is the kappa-mechanism operating in the hydrogen and the helium partial ionization regions. One of the most significant problems in the analysis is the effect of convection on both the pulsation and structure of the envelopes. The radial blue edge is about 1,000 K hotter than the nonradial blue edge, while the radial red edge is cooler than the nonradial red edge.

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