Astronomy and Astrophysics – Astrophysics
Scientific paper
Jun 1987
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987apj...317..303c&link_type=abstract
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 317, June 1, 1987, p. 303-324. DOE-supported research.
Astronomy and Astrophysics
Astrophysics
42
Helium, Hydrogen, Stellar Models, Stellar Oscillations, Surface Layers, White Dwarf Stars, Hot Stars, Stellar Temperature
Scientific paper
Models for DA white dwarf stars with effective temperatures between 9000 and 12,000 K and models for DB white dwarfs with effective temperatures of 25,000 K and 27,000 K have been tested for stability against both radial and nonradial pulsations. The construction of the models is discussed, and linear nonadiabatic nonradial pulsation results for these models are given assuming frozen-in convection. The time variation of convection is simulated in a crude way, and it is shown that many unstable modes can be completely stabilized. The results show that thick hydrogen shells can produce nonradial pulsations and that the existence of convection blocking exists for both radial and nonradial modes in DA and DB white dwarf stars. It is found that convection at the surface of white dwarfs must be very efficient in order for the theoretical nonradial instability strip to have a blue edge hot enough to agree with observations.
Cox Arthur N.
Kidman Russell B.
Pesnell William Dean
Starrfield Sumner G.
No associations
LandOfFree
Pulsations of white dwarf stars with thick hydrogen or helium surface layers 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 Pulsations of white dwarf stars with thick hydrogen or helium surface layers, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and Pulsations of white dwarf stars with thick hydrogen or helium surface layers will most certainly appreciate the feedback.
Profile ID: LFWR-SCP-O-1813934