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 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 کاملGeneralized pulsating strings
In this paper we consider new solutions for pulsating strings. For this purpose we use the idea of the generalized ansatz for folded and circular strings in hep-th/0311004. We find the solutions to the resulting Neumann-Rosochatius integralbe system and the corrections to the energy. To do that we use the approach developed by Minahan in hep-th/0209047 and find that the corrections are quite di...
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 young brown dwarfs
We present the results of a nonadiabatic, linear stability analysis of models of very low-mass stars (VLMSs) and brown dwarfs (BDs) during the deuterium burning phase in the center. We find unstable fundamental modes with periods varying between ∼5 hr for a 0.1 M⊙ star and ∼1 hr for a 0.02 M⊙ BD. The growth time of the instability decreases with decreasing mass and remains well below the deuter...
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ژورنال
عنوان ژورنال: The Lancet
سال: 1890
ISSN: 0140-6736
DOI: 10.1016/s0140-6736(01)85856-6