Analysis of radiation pressure effects in pulsating stars through perturbative limit cycle solutions
نویسندگان
چکیده
منابع مشابه
Observations of Pulsating Stars
Pulsations discussed will begin at the “top” of the instability strip with pulsating red giants and Miras, which are evolved stars nearing their own demise. The next discussed will be the Cepheids, both the “Classical” ones as well as the W Virginis (Population II stars). While moving down the instability strip of the HR Diagram, the next major type of variable (pulsating) star are the RR Lyrae...
متن کاملModal Selection In Pulsating Stars
Initial-value and periodic nonlinear pulsation integrations are carried out for a series of doublemode Cepheid models (PdPo 0.7) in the vicinity of the resonance WI + Wo = W3. None of the models tested shows persistent double-mode behavior. A new, semiquantitative description of modal selection, based upon the iterative theory of Simon, is introduced to analyze the nonlinear results. In the sim...
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Pulsating stars have given important information in classical astronomy and are still an active research field, e.g. asteroseismology or helioseismology. By studying the rich oscillation stellar spectra, optical astronomy makes predictions for the stellar equations of state (EOS), the evolutionary age of the stars, and in the case of Cepheids one can make exact predictions for the distance of t...
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This REU summer project dealt mainly with analyzing data and determining the periods of certain types of pulsating variable stars called RR Lyraes and Cepheids. Pulsating variables periodically change in brightness over a certain amount of time for reasons having to do with the internal structure of the star itself. Dr. Horace Smith has been studying such variables in our neighboring galaxy, th...
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Even when we consider Newtonian stars, i.e., stars with surface gravitational redshift, z ≪ 1, it is well known that, theoretically, it is possible to have stars, supported against self-gravity, almost entirely by radiation pressure. However, such Newtonian stars must necessarily be supermassive(Weinberg 1972).We point out that this requirement for excessive large M , in Newtonian case, is a co...
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ژورنال
عنوان ژورنال: The Astrophysical Journal
سال: 1991
ISSN: 0004-637X,1538-4357
DOI: 10.1086/170042