Pulsations of white dwarf stars with thick hydrogen or helium surface layers

Details Pulsations of white dwarf stars with thick hydrogen or helium surface layers Pulsations of white dwarf stars with thick hydrogen or helium surface layers

Jul 1986

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1986stin...8721774c&link_type=abstract

Presented at the IUA Symposium No. 123, Aarhus, Denmark, 7 Jul. 1986

Physics

Helium, Hydrogen, Surface Layers, Surface Properties, White Dwarf Stars, Convection, Pulses, Unsteady Flow

Scientific paper

In order to see if there could be agreement between results of stellar evolution theory and those of nonradial pulsation theory, calculations of white dwarf models have been made for hydrogen surface masses of 10 to the -4 solar masses. Earlier results indicated that surface masses greater than 10 to the -8 solar masses would not allow nonradial pulsations, even though all the driving and damping is in surface layers only 10 to the -12 of the mass thick. It is shown that the surface mass of hydrogen in the pulsating white dwarfs (ZZ Ceti variables) can be any value as long as it is thick enough to contain the surface convection zone.

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