Relativistic, Spherically Symmetric Star Clusters. III. Stability of Compact Isotropic Models

1969 ◽  
Vol 158 ◽  
pp. 17 ◽  
Author(s):  
James R. Ipser
Keyword(s):  
Star Clusters ◽  
Spherically Symmetric ◽  
Symmetric Star

Odd-parity perturbations of spherically symmetric star clusters in general relativity

1981 ◽  
Vol 247 ◽  
pp. 671 ◽  
Author(s):  
R. Semenzato ◽  
J. R. Ipser
Keyword(s):  
General Relativity ◽  
Star Clusters ◽  
Spherically Symmetric ◽  
Symmetric Star

scholarly journals Compact Nuclei of Galaxies and Sources of Their Energy

1999 ◽  
Vol 194 ◽  
pp. 323-323
Author(s):  
L.Sh. Grigoryan ◽  
G.S. Sahakian
Keyword(s):  
Equation Of State ◽  
Star Clusters ◽  
Galactic Nuclei ◽  
Star Cluster ◽  
Statistical Equilibrium ◽  
Spherically Symmetric ◽  
Symmetric Star ◽  
Age Of The Universe ◽  
The Universe

A model of compact nuclei of galaxies as spherically-symmetric star clusters is proposed. A concept of the equation of state for star clusters in statistical equilibrium is introduced (galactic nuclei are systems in statistical equilibrium if their age is of the order of the age of the Universe). It is shown that a statistically equilibrium star cluster is described by the equation of state of a polytrope P = aρ3, and with its help the main parameters of compact nuclei of galaxies are calculated. The formula M = 2.524GR5/a for mass M and radius R of the cluster is derived.

scholarly journals The Concentric Shell Method for Relativistic Star Clusters

1975 ◽  
Vol 69 ◽  
pp. 433-439 ◽  
Author(s):  
E. D. Fackerell
Keyword(s):  
Star Clusters ◽  
Spherically Symmetric ◽  
Spherical Shells ◽  
Relativistic Star ◽  
Symmetric Star ◽  
Concentric Shell

The analytic aspects of the Campbell-Hénon method of concentric spherical shells are generalized for application to relativistic spherically symmetric star clusters.

Relativistic, Spherically Symmetric Star Clusters. I. Stability Theory for Radial Perturbations

1968 ◽  
Vol 154 ◽  
pp. 251 ◽  
Author(s):  
James R. Ipser ◽  
Kip S. Thorne
Keyword(s):  
Stability Theory ◽  
Star Clusters ◽  
Spherically Symmetric ◽  
Symmetric Star

scholarly journals EXPANSIONFREE FLUID EVOLUTION AND SKRIPKIN MODEL IN f(R) THEORY

2011 ◽  
Vol 20 (11) ◽  
pp. 2239-2252 ◽  
Author(s):  
M. SHARIF ◽  
H. RIZWANA KAUSAR
Keyword(s):  
General Relativity ◽  
The Self ◽  
Spherically Symmetric ◽  
Junction Conditions ◽  
Dynamical Equations ◽  
Constant Energy ◽  
Isotropic Pressure ◽  
Symmetric Star ◽  
Constant Energy Density ◽  
General Influence

We consider the modified f(R) theory of gravity whose higher-order curvature terms are interpreted as a gravitational fluid or dark source. The gravitational collapse of a spherically symmetric star, made up of locally anisotropic viscous fluid, is studied under the general influence of the curvature fluid. Dynamical equations and junction conditions are modified in the context of f(R) dark energy and by taking into account the expansionfree evolution of the self-gravitating fluid. As a particular example, the Skripkin model is investigated which corresponds to isotropic pressure with constant energy density. The results are compared with corresponding results in General Relativity.

Gravitational collapse of dark matter interacting with dark energy: Black hole formation

2017 ◽  
Vol 26 (13) ◽  
pp. 1750142 ◽  
Author(s):  
Hasrat Hussain Shah ◽  
Quaid Iqbal
Keyword(s):  
Black Hole ◽  
Dark Matter ◽  
Dark Energy ◽  
Gravitational Collapse ◽  
Anisotropic Pressure ◽  
Spherically Symmetric ◽  
Hole Formation ◽  
White Hole ◽  
De Formula ◽  
Symmetric Star

In this work, we study the gravitational collapsing process of a spherically symmetric star constitute of Dark Matter (DM), [Formula: see text], and Dark Energy (DE) [Formula: see text]. In this model, we use anisotropic pressure with Equation of State (EoS) [Formula: see text] and [Formula: see text], [Formula: see text]. It reveals that gravitational collapse of DM and DE with interaction leads to the formation of the black hole. When [Formula: see text] (phantoms), dust and phantoms could be ejected from the death of white hole. This emitted matter again undergoes to collapsing process and becomes the black hole. This study gives the generalization for isotropy of pressure in the fluid to anisotropy when there will be interaction between DM and DE.

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