Stability of dense stellar clusters to relativistic collapse is investigated by an approximate method, similar to static criteria of stellar stability. The equilibrium models with a Maxwellian distribution function and cutoff, studied by Zel'dovich and Podurets (ZP), have been considered. The method considers a simple non-Maxwellian distribution function, obtained from the Maxwellian one by the condition of conservation of adiabatic invariant during non collisional perturbations. The method considered here gives results coincident with the ones carried out by the method based on sequences at constant entropy. These results are better than ones obtained from considerations of the sequence of Maxwellian models with different temperature, made by ZP. In particular they are much closer to the results of the numerical simulations of Shapiro and Teukolsky.
Stability of the dense stellar clusters - I / BISNOVATYI KOGAN, G. S.; Merafina, Marco; Ruffini, Remo; Vesperini, E.. - In: PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC. - ISSN 0004-6280. - STAMPA. - 48:(1993), pp. 705-708.
Stability of the dense stellar clusters - I
MERAFINA, MarcoWriting – Original Draft Preparation
;RUFFINI, Remo;
1993
Abstract
Stability of dense stellar clusters to relativistic collapse is investigated by an approximate method, similar to static criteria of stellar stability. The equilibrium models with a Maxwellian distribution function and cutoff, studied by Zel'dovich and Podurets (ZP), have been considered. The method considers a simple non-Maxwellian distribution function, obtained from the Maxwellian one by the condition of conservation of adiabatic invariant during non collisional perturbations. The method considered here gives results coincident with the ones carried out by the method based on sequences at constant entropy. These results are better than ones obtained from considerations of the sequence of Maxwellian models with different temperature, made by ZP. In particular they are much closer to the results of the numerical simulations of Shapiro and Teukolsky.I documenti in IRIS sono protetti da copyright e tutti i diritti sono riservati, salvo diversa indicazione.