On the existence of stable relativistic star clusters with arbitrarily large central redshifts

1989 ◽  
Vol 336 ◽  
pp. L63 ◽  
Author(s):  
Frederic A. Rasio ◽  
Stuart L. Shapiro ◽  
Saul A. Teukolsky
Keyword(s):  
Star Clusters ◽  
Relativistic Star

Relativistic star clusters with high central redshift

Pramana ◽  
1980 ◽  
Vol 15 (1) ◽  
pp. 53-63
Author(s):  
M C Durgapal ◽  
P S Rawat ◽  
R Banerji
Keyword(s):  
Star Clusters ◽  
Relativistic Star

The dynamic instability of isothermal relativistic star clusters

1976 ◽  
Vol 203 ◽  
pp. 477 ◽  
Author(s):  
K. G. Suffern ◽  
E. D. Fackerell
Keyword(s):  
Dynamic Instability ◽  
Star Clusters ◽  
Relativistic Star

Relativistic Stellar Dynamics in Rotating Axially Symmetric Systems

1968 ◽  
Vol 1 (3) ◽  
pp. 86-87 ◽  
Author(s):  
E.D. Fackerell
Keyword(s):  
General Relativity ◽  
Star Clusters ◽  
Stellar Dynamics ◽  
Spherically Symmetric ◽  
Axially Symmetric ◽  
Relativistic Star ◽  
General Relativistic ◽  
Stellar Sources ◽  
Symmetric Systems

Recently the possibility has been raised of using general relativistic star clusters as models for quasi-stellar sources. The theory of static, spherically symmetric, collisionless star clusters has been developed within the framework of general relativity. In particular, analogues have been found of the Newtonian polytropic models and of Woolley’s truncated Maxwellian systems. However, in view of the importance of rotation on stability in relativistic astrophysical problems, it is of considerable interest to include the effect of rotation in relativistic stellar dynamics.

scholarly journals The Structure and Dynamic Instability of Isothermal Relativistic Star Clusters

1976 ◽  
Vol 29 (4) ◽  
pp. 311 ◽  
Author(s):  
Edward D Fackerell ◽  
Kevin G Suffern
Keyword(s):  
Dynamic Stability ◽  
Dynamic Instability ◽  
Rest Mass ◽  
Star Clusters ◽  
Relativistic Star ◽  
The Stability

The structure and dynamic stability of isothermal relativistic star clusters are discussed both for the case of clusters without dispersion in stellar rest mass and for two families of clusters with dispersion in stellar rest mass. We show that the former are dynamically unstable if the central redshift is greater than about 0'5, and that the latter are dynamically unstable if the central redshift is greater than about O' 6, so that the inclusion of dispersion in mass does not greatly affect the stability of isothermal relativistic star clusters.

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.

scholarly journals Solving Einstein's equations for rotating spacetimes: Evolution of relativistic star clusters

1994 ◽  
Vol 49 (10) ◽  
pp. 5153-5164 ◽  
Author(s):  
Andrew M. Abrahams ◽  
Gregory B. Cook ◽  
Stuart L. Shapiro ◽  
Saul A. Teukolsky
Keyword(s):  
Star Clusters ◽  
Einstein’S Equations ◽  
Einstein's Equations ◽  
Relativistic Star
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