| Full text | |
| Author(s): |
Total Authors: 2
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| Affiliation: | [1] Silesian Univ Opava, Fac Philosophy & Sci, Inst Phys, Bezrucovo Nam 13, CZ-74601 Opava - Czech Republic
[2] Silesian Univ Opava, Res Ctr Theoret Phys & Astrophys, Bezrucovo Nam 13, CZ-74601 Opava - Czech Republic
[3] Univ Fed Abc, Ctr Math Computat & Cognit, Av Estados 5001, BR-09210580 Santo Andre, SP - Brazil
Total Affiliations: 3
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| Document type: | Journal article |
| Source: | Classical and Quantum Gravity; v. 36, n. 6 MAR 21 2019. |
| Web of Science Citations: | 5 |
| Abstract | |
In this paper we used the theory of adiabatic radial oscillations developed by Chandrasekhar to study the conditions for dynamical stability of constant energy-density stars, or Schwarzschild stars, in the unstudied ultra compact regime beyond the Buchdahl limit, that is, for configurations with radius R in the range R-S < R < (9/8)R-S, where R-S is the Schwarzschild radius of the star. These recently found analytical solutions exhibit a negative pressure region in their centre and, in the limit when R -> R-S, the full interior region of the star becomes filled with negative pressure. Here we present a systematic analysis of the stability of these configurations against radial perturbations. We found that, contrary to the usual expectation found in many classical works, the ultra compact Schwarzschild star is stable against radial oscillations. We computed values of the critical adiabatic index gamma(c) for several stellar models with varying radius R/Rs and found that it also approaches a finite value as R/R-S -> 1. (AU) | |
| FAPESP's process: | 15/50421-8 - Gravitational waves and neutron star oscillations |
| Grantee: | Cecilia Bertoni Martha Hadler Chirenti |
| Support Opportunities: | Regular Research Grants |