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

Conference · Tue Jul 01 00:00:00 EDT 1986

OSTI ID:6976610

Cox, A N; Starrfield, S G; Kidman, R B; Pesnell, W D

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/sup -4/ solar masses. Earlier results indicated that surface masses greater than 10/sup -8/ solar masses would not allow nonradial pulsations, even though all the driving and damping is in surface layers only 10/sup -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. 10 refs., 6 figs.

• Research Organization: Los Alamos National Laboratory (LANL), Los Alamos, NM (United States)
• DOE Contract Number: W-7405-ENG-36
• OSTI ID: 6976610
• Report Number(s): LA-UR-86-3395; CONF-8607108-1; ON: DE87001954
• Resource Relation: Conference: 123. symposium of the International Astronomical Union, Aarhus, Denmark, 7 Jul 1986; Other Information: Portions of this document are illegible in microfiche products
• Country of Publication: United States
• Language: English

Related Subjects

71 CLASSICAL AND QUANTUM MECHANICS
GENERAL PHYSICS
WHITE DWARF STARS
PULSATIONS
CONVECTION
HELIUM
HYDROGEN
SURFACE PROPERTIES
THEORETICAL DATA
DATA
DWARF STARS
ELEMENTS
ENERGY TRANSFER
FLUIDS
GASES
HEAT TRANSFER
INFORMATION
MASS TRANSFER
NONMETALS
NUMERICAL DATA
RARE GASES
STARS
640102* - Astrophysics & Cosmology- Stars & Quasi-Stellar
Radio & X-Ray Sources