منابع مشابه
8 - Stellar Pulsation and Oscillation
That some stars vary in brightness has been known from time immemorial. That this variation is the result of intrinsic changes in the star itself has been known for less than 100 years and the causes of those variations have been understood for less than 30 years. It is not a simple matter to distinguish the light variations resulting from eclipses by a companion from those caused by physical c...
متن کاملObservations of the pulsation of the Cepheid l Car with the Sydney University Stellar Interferometer
Observations of the southern Cepheid ℓ Car to yield the mean angular diameter and angular pulsation amplitude have been made with the Sydney University Stellar In-terferometer (SUSI) at a wavelength of 696 nm. The resulting mean limb-darkened angular diameter is 2.990±0.017 mas (i.e. ±0.6 per cent) with a maximum-to-minimum amplitude of 0.560±0.018 mas corresponding to 18.7±0.6 per cent in the ...
متن کاملCepheid models based on self-consistent stellar evolution and pulsation calculations: the right answer?
We have computed stellar evolutionary models for stars in a mass range characteristic of Cepheid variables (3 < m/M < 12) for different metallicities representative of the Galaxy and the Magellanic Clouds populations. The stellar evolution calculations are coupled to a linear non adiabatic stability analysis to get self-consistent mass-period-luminosity relations. The period luminosity relation...
متن کاملPulsation modes in rapidly rotating stellar models based on the Self-Consistent Field method
Context. New observational means such as the space missions CoRoT and Kepler and ground-based networks are and will be collecting stellar pulsation data with unprecedented accuracy. A significant fraction of the stars in which pulsations are observed are rotating rapidly. Aims. Our aim is to characterise pulsation modes in rapidly rotating stellar models so as to be able to interpret asteroseis...
متن کاملEffects of moderate rotation on stellar pulsation I. Third order perturbation formalism
Interpretation of the available ground-based and forthcoming space observations of multiperiodic variable stars require accurate computations of oscillation frequencies. Typical rotational equatorial velocities of upper main sequence stars range between 50 and 200 km/s and the effect of rotation on the oscillation frequencies of these stars must be included. The rotation can still be considered...
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ژورنال
عنوان ژورنال: Reviews of Modern Physics
سال: 1964
ISSN: 0034-6861
DOI: 10.1103/revmodphys.36.555