On the Pulsational Stability of Stars with Convective Envelopes.

1957 ◽  
Vol 126 ◽  
pp. 386 ◽  
Author(s):  
Irving N. Rabinowitz
Keyword(s):  
Stability Of Stars ◽  
Pulsational Stability

Pulsational Stability of Stars in Thermal Imbalance

1973 ◽  
Vol 182 ◽  
pp. 885 ◽  
Author(s):  
J. P. Cox ◽  
C. J. Hansen ◽  
William R. Davey
Keyword(s):  
Stability Of Stars ◽  
Thermal Imbalance ◽  
Pulsational Stability

Influence of Convection on the Pulsational Stability of Stars

1981 ◽  
Vol 93 ◽  
pp. 278-279
Author(s):  
Y. Osaki ◽  
G. Gonczi
Keyword(s):  
Time Dependent ◽  
Phase Lag ◽  
Instability Strip ◽  
Convective Flux ◽  
Local Character ◽  
Spatial Oscillations ◽  
Stability Of Stars ◽  
Mixing Length Theory ◽  
Astronomy And Astrophysics ◽  
Pulsational Stability

Influence of convection on the pulsational stability of stars is examined based on Unno's (1967) theory of time-dependent convection. This theory is an extension of Vitense's local mixing-length theory of convection to the time-dependent problem. The equations of linear non-adiabatic pulsations, which include the thermal interaction between convection and pulsation, have been solved numerically on a series of Cepheid models. It is found that the thermal eigenfunctions (of δ T/T and δ L/L) exhibit spatial oscillations with short wavelength in cool stellar models where the energy is mostly transported by convection. This phenomenon of spatial oscillations is interpreted, and it is shown that they arise because of the phase lag of the convective flux to pulsation and they are related to the local character of the convection theory. It is found that the spatial oscillations play a determinant role in the pulsational stability in the region of the red edge of the Cepheid instability strip, as far as the thermal convection-pulsation coupling is concerned. The details of this study have been pulbished in Astronomy and Astrophysics.

Impact of f(R,T) gravity in evolution of charged viscous fluids

2021 ◽  
Vol 30 (04) ◽  
pp. 2150027
Author(s):  
I. Noureen ◽  
Usman-ul-Haq ◽  
S. A. Mardan
Keyword(s):  
Stability Analysis ◽  
Energy Momentum Tensor ◽  
Momentum Tensor ◽  
Viscous Fluids ◽  
Fluid Distribution ◽  
Perturbation Scheme ◽  
Field Equations ◽  
Dynamical Equations ◽  
Stability Of Stars ◽  
The Stability

In this work, the evolution of spherically symmetric charged anisotropic viscous fluids is discussed in framework of [Formula: see text] gravity. In order to conduct the analysis, modified Einstein Maxwell field equations are constructed. Nonzero divergence of modified energy momentum tensor is taken that implicates dynamical equations. The perturbation scheme is applied to dynamical equations for stability analysis. The stability analysis is carried out in Newtonian and post-Newtonian limits. It is observed that charge, fluid distribution, electromagnetic field, viscosity and mass of the celestial objects greatly affect the collapsing process as well as stability of stars.

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