Anisotropic Stars II: Stability
By Krsna Dev, M. Gleiser. 2003
182 citations recorded by the source corpus.
We investigate the stability of self-gravitating spherically symmetric anisotropic spheres under radial perturbations. We consider both the Newtonian and the full general-relativistic perturbation treatment. In the general-relativistic case, we extend the variational formalism for spheres with isotropic pressure developed by Chandrasekhar. We find that, in general, when the tangential pressure is greater than the radial pressure, the stability of the anisotropic sphere is enhanced when compared to isotropic configurations. In particular, anisotropic spheres are found to be stable for smaller values of the adiabatic index γ.
Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics
View Paper: https://www.semanticscholar.org/paper/810bf8215e6c6b5b3ee42ef8acd3d3ca14e202ac
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In Nuclear and High Energy Physics
Citations in the corpus
- Sound speeds, cracking and the stability of self-gravitating anisotropic compact objects (2007, methodology): “Other types of perturbations leading to expanding or collapsing evolutions could be considered in the standard Chandrasekhar’s variational formalism ( see [8,9] and references therein).”
- Radial pulsations and stability of anisotropic stars with a quasi-local equation of state (2010, methodology): “In the context of anisotropic stars the normal modes technique was applied to study the stability of some specific configurations in [16] and also [17, 18].”
- How to tell a gravastar from a black hole (2007, background): “This is no longer true for polar perturbations (for which the pressure anisotropy plays an important role) and a study on radial perturbations of stars with anisotropi c pressures was recently presented in [19, 20 ].”