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Linear radial pulsation theory. Lecture 5 [electronic resource].

Published:
Los Alamos, N.M. : Los Alamos National Laboratory, 1983.
Oak Ridge, Tenn. : Distributed by the Office of Scientific and Technical Information, U.S. Dept. of Energy.
Physical Description:
Pages: 11 : digital, PDF file
Additional Creators:
Los Alamos National Laboratory and United States. Department of Energy. Office of Scientific and Technical Information
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Summary:
We describe a method for getting an equilibrium stellar envelope model using as input the total mass, the envelope mass, the surface effective temperature, the total surface luminosity, and the composition of the envelope. Then wih the structure of the envelope model known, we present a method for obtaining the raidal pulsation periods and growth rates for low order modes. The large amplitude pulsations observed for the yellow and red giants and supergiants are always these radial models, but for the stars nearer the main sequence, as for all of our stars and for the white dwarfs, there frequently are nonradial modes occuring also. Application of linear theory radial pulsation theory is made to the giant star sigma Scuti variables, while the linear nonradial theory will be used for the B stars in later lectures.
Report Numbers:
E 1.99:la-ur-83-785
E 1.99: conf-830337-5
conf-830337-5
la-ur-83-785
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Note:
Published through SciTech Connect.
01/01/1983.
"la-ur-83-785"
" conf-830337-5"
"DE83010093"
Swiss Society of Astrophysics and Astronomy conference, Saas Fee, Switzerland, 21 Mar 1983.
Cox, A.N.
Funding Information:
W-7405-ENG-36
View MARC record | catkey: 13826674