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 کاملPulsating Relativistic Stars
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...
متن کاملPulsating Variable Stars
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...
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...
متن کاملA fresh look into pulsating PG1159 stars
To improve the understanding of the pulsational instabilities of some of the PG1159-type pre-white dwarfs we performed detailed stability analyses on helium star evolutionary models. With the canonical chemical compositions, pulsational instabilities were encountered for all stellar masses considered (0.57, 0.63, 0.7 M⊙). The blue boundary agrees satisfactorily with observations. The red edge, ...
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ژورنال
عنوان ژورنال: Nature
سال: 1948
ISSN: 0028-0836,1476-4687
DOI: 10.1038/162934a0