Radial pulsations and stability of anisotropic stars with a quasi-local equation of state
By D. Horvat, S. Ilijić, A. Marunovi'c. 2010
143 citations recorded by the source corpus.
Quasi-local variables, i.e. quantities whose values can be derived from physics accessible within an arbitrarily small neighborhood of a spacetime point, are used to construct the equation of state (EoS) for the anisotropic fluid in the spherical symmetry. One parameter families of equilibrium solutions are obtained making it possible to assess stability properties by means of the standard M(R) method. Normal modes of radial pulsation are computed as well and are found to confirm the onset of instability as predicted by the M(R) method. As an example, a stable configuration with outwardly increasing energy density in the core is obtained with a simple quasi-local extension of the polytropic EoS. It is also found that the loss of stability occurs at higher surface compactness when the anisotropy of pressures is present.
Subfields: Astronomy and Astrophysics, Oceanography
View Paper: https://www.semanticscholar.org/paper/8f1874b522c8edf42793c512b009904c301dd50b
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In Astronomy and Astrophysics
- Diego Rubiera-García
- Kent Yagi
- Aneta Wojnar
- N. Yunes
- G. Olmo
- Lavinia Heisenberg
- Jose Beltrán Jiménez
- Luciano Rezzolla
In Oceanography
Citations in the corpus
- Stellar structure models in modified theories of gravity: Lessons and challenges (2019, background): “ting stars of scalar-tensor theories in the Einstein frame (20) has been investigated by Silva et al. [390]. Within GR, these effects may increase the maximum allowed neutron star mass for a given EOS [239]. Assumingagainadependence(110)andfocusingontheAPREOSfortheradialpressureP r,andtheHorvat(99),a”
- Approximate Universal Relations for Neutron Stars and Quark Stars (2016, background): “r that is spacelike (k k = 1) and orthogonal to u (k u = 0). The choice of how pdiers from q tdenes the anisotropy model. Yagi and Yunes [223] mainly considered the one proposed by Horvat et al. [225] (H model), in which the dierence between radial and tangential pressures in a spherically-symmetric”