Stability of thin-shell interfaces inside compact stars

Pereira, Jonas P.; Coelho, Jaziel G.; Rueda, J. A.

doi:10.1103/physrevd.90.123011

Cited by 18 publications

(12 citation statements)

References 46 publications

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“…The fourdimensional MIT bag model equation of state was considered in some previous investigations on structure and stability against radial perturbations, for example, to investigate the radial pulsations in Refs. [25][26][27][28][29] and the stability of thin shell interfaces within compact stars [30] (see also Refs. [31,32]).…”

Section: Equation Of Statementioning

confidence: 99%

Extra dimensions’ influence on the equilibrium and radial stability of strange quark stars

et al. 2019

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We analyze the influence of extra dimensions on the static equilibrium configurations and stability against radial perturbations. For this purpose, we solve stellar structure equations and radial perturbation equations, both modified for a d-dimensional spacetime (d ≥ 4) considering that spacetime outside the object is described by a Schwarzschild-Tangherlini metric. These equations are integrated considering a MIT bag model equation of state extended for d ≥ 4. We show that the spacetime dimension influences both the structure and stability of compact objects. For an interval of central energy densities ρ cd G d and total masses M G d /(d − 3), we show that the stars gain more stability when the dimension is increased. In addition, the maximum value of M G d /(d − 3) and the zero eigenfrequency of oscillation are found with the same value of ρ cd G d ; i.e., the peak value of M G d /(d − 3) marks the onset of instability. This indicates that the necessary and sufficient conditions to recognize regions constructed by stable and unstable equilibrium configurations against radial perturbations are, respectively, dM/dρ cd > 0 and dM/dρ cd < 0. We obtain that some physical parameter of the compact object in a d-dimensional spacetime, such as the radius and the mass, depend of the normalization. Finally, within the Newtonian framework, the results show that compact objects with adiabatic index Γ1 ≥ 2(d − 2)/(d − 1) are stable against small radial perturbations. * Electronic address: jose.arbanil@upn.pe † Electronic address: araujogc@ita.br ‡ Electronic address: rvlobato@ita.br § Electronic address: marinho@ita.br ¶ Electronic address: malheiro@ita.br arXiv:1907.07661v1 [gr-qc]

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Section: Equation Of Statementioning

confidence: 99%

Extra dimensions’ influence on the equilibrium and radial stability of strange quark stars

et al. 2019

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“…where the prime operation has been defined as the radial derivative. Actually, σ and P are not independent, but are related through (Pereira et al 2014;Lobo and Crawford 2005)…”

Section: Thin Shell Formalism In the Spherical Casementioning

confidence: 99%

“…Given that σ and P have intrinsic general relativistic terms (Pereira et al 2014), they are not the usual (laboratory) surface energy density and usual surface tension, respectively. Thus, it seems reasonable to call P the "thin shell surface tension" and σ the "thin shell surface energy density".…”

Section: Thin Shell Formalism In the Spherical Casementioning

confidence: 99%

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General Relativistic Surface Degrees of Freedom in Perturbed Hybrid Stars

Pereira

Lugones²

2019

ApJ

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We study how the nature of a hybrid system (perfect fluid, solid or a mixture of them) could be related to the induction of general relativistic surface degrees of freedom on phase-splitting surfaces upon perturbation of its phases. We work in the scope of phase conversions in the vicinity of sharp phase transition surfaces whose timescales are either much smaller (rapid conversions) or larger (slow conversions) than the ones of the perturbations (ω −1 , where ω is a characteristic frequency of oscillation of the star). In this first approach, perturbations are assumed to be purely radial. We show that surface degrees of freedom could emerge when either the core or the crust of a hybrid star is solid and phase conversions close to a phase-splitting surface are rapid. We also show how this would change the usual stability rule for solid hybrid stars, namely ∂M 0 /∂ρ c ≥ 0, where M 0 is the total mass to the background hybrid star and ρ c its central density. Further consequences of our analysis for asteroseismology are also briefly discussed.

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“…We assume that the radial pressure and fluid energy density are connected by the MIT bag model equation of state. This equation of state was used in previous works, for instance, to study the radial oscillations of strange stars [20][21][22] and the stability of thin shell interfaces inside compact stars [23] (review also [24]). In turn, the anisotropic equation of state will be described by two possibles cases, one that follows the function σ = α (p r + ρ) (ρ + 3 p r ) e λ r 2 and another one of the form σ = β p r (1 − e λ ).…”

Section: Introductionmentioning

confidence: 99%

Radial stability of anisotropic strange quark stars

Arbañil

Malheiro

2016

J. Cosmol. Astropart. Phys.

106

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Abstract. The influence of the anisotropy in the equilibrium and stability of strange stars is investigated through the numerical solution of the hydrostatic equilibrium equation and the radial oscillation equation, both modified from their original version to include this effect. The strange matter inside the quark stars is described by the MIT bag model equation of state. For the anisotropy two different kinds of local anisotropic σ = p t − p r are considered, where p t and p r are respectively the tangential and the radial pressure: one that is null at the star's surface defined by p r (R) = 0, and one that is nonnull at the surface, namely, σ s = 0 and σ s = 0. In the case σ s = 0, the maximum mass value and the zero frequency of oscillation are found at the same central energy density, indicating that the maximum mass marks the onset of the instability. For the case σ s = 0, we show that the maximum mass point and the zero frequency of oscillation coincide in the same central energy density value only in a sequence of equilibrium configurations with the same value of σ s . Thus, the stability star regions are determined always by the condition dM/dρ c > 0 only when the tangential pressure is maintained fixed at the star surface's p t (R). These results are also quite important to analyze the stability of other anisotropic compact objects such as neutron stars, boson stars and gravastars.arXiv:1607.03984v2 [astro-ph.HE]

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Stability of thin-shell interfaces inside compact stars

Cited by 18 publications

References 46 publications

Extra dimensions’ influence on the equilibrium and radial stability of strange quark stars

Extra dimensions’ influence on the equilibrium and radial stability of strange quark stars

General Relativistic Surface Degrees of Freedom in Perturbed Hybrid Stars

Radial stability of anisotropic strange quark stars

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