Analytical study of anisotropic compact star models

Иванов, Б. В.

doi:10.1140/epjc/s10052-017-5322-7

Cited by 89 publications

(105 citation statements)

References 112 publications

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“…more recently this equivalence between the restriction on pressures and velocities was demonstrated in [16] and included as part of the acceptability conditions that have to be considered when building physically reasonable compact object models. We shall discuss these constraints in the next section.…”

Section: Convection and Cracking Sources Of Instabilitymentioning

confidence: 99%

“…Additionally B.V Ivanov [16], demonstrated that these conditions are not independent and can be condensed in five main inequalities:…”

Section: Physical Acceptability Conditionsmentioning

confidence: 99%

“…Within the global stability criteria we can also identify the Harrison-Zeldovich-Novikov condition, which implies that dM (ρ c )/dρ c ≥ 0, where M is the total mass of the configuration and ρ c the central density, of the distribution [16]. The stability of a spherical star to convection implies the buoyancy principle which leads to that pressure and energy density must, decrease outwards in any hydrostatic matter configuration [17][18][19].…”

Section: Introductionmentioning

confidence: 99%

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Convection and cracking stability of spheres in general relativity

2018

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In the present paper we consider convection and cracking instabilities as well as their interplay. We develop a simple criterion to identify equations of state unstable to convection, and explore the influence of buoyancy on cracking (or overturning) for isotropic and anisotropic relativistic spheres. We show that a density profile ρ(r), monotonous, decreasing and concave , i.e. ρ < 0 and ρ < 0, will be stable against convection, if the radial sound velocity monotonically decreases outward. We also studied the cracking instability scenarios and found that isotropic models can be unstable, when the reaction of the pressure gradient is neglected, i.e. δRp = 0; but if it is considered, the instabilities may vanish and this result is valid, for both isotropic and anisotropic matter distributions. * hector@ula.ve †

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Section: Convection and Cracking Sources Of Instabilitymentioning

confidence: 99%

“…Additionally B.V Ivanov [16], demonstrated that these conditions are not independent and can be condensed in five main inequalities:…”

Section: Physical Acceptability Conditionsmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Convection and cracking stability of spheres in general relativity

2018

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“…In the literature y is given and a 1 is found from Eq (32) [30], [31], [32], [33], [34], [35], [36], [37], [38], [39]. Due to Eqs (6, 7) one finds quickly y form µ or m. Solutions with LEOS and known µ are given in [40], [41], [42] and [43].…”

Section: Types Of Equationsmentioning

confidence: 99%

Linear and Riccati equations in generating functions for stellar models in general relativity

Иванов

2020

Eur. Phys. J. Plus

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It is shown that the expressions for the tangential pressure, the anisotropy factor and the radial pressure in the Einstein equations may serve as generating functions for stellar models. The latter can incorporate an equation of state when the expression for the energy density is also used. Other generating functions are based on the condition for the existence of conformal motion (conformal flatness in particular) and the Karmarkar condition for embedding class one metrics. In all these cases the equations are linear first order differential equations for one of the metric components and Riccati equations for the other. The latter may be always transformed into second order homogenous linear differential equations. These conclusions are illustrated by numerous particular examples from the study of stellar models.

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“…where ǫ denotes the total-energy density, p the radial pressure, and c s the radial sound speed, respectively [40].…”

Section: The Conservation Of Baryon Numbermentioning

confidence: 99%

Effect of viscosity and thermal conductivity on the radial oscillation and relaxation of relativistic stars

Bárta¹

2019

Class. Quantum Grav.

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In this paper we present a generic formulation of the linearized dynamical equations governing small adiabatic radial oscillations of relativistic stars. The dynamical equations are derived by taking into consideration those effects of viscosity and thermal conductivity of neutron-star matter which directly determine the minimum period of observable pulsars. A variational principle is applied to determine a discrete set of eigenfunctions with complex eigenvalues. The real and imaginary parts of eigenvalues represent the squared natural frequencies and relaxation time of radial oscillations of non-rotating neutron stars, respectively. We provide a suitable framework which may be supplemented with various potential species of cold-nuclearmatter models to compute the spectra of the normalized eigenfrequencies with a certain numerical precision. In the last section, we provide a qualitative estimation of the rate at which viscosity and thermal conductivity drain the kinetic energy of radial oscillation mode in reasonably uniform neutron stars, without relying on explicit numerical computations.Effect of viscosity and thermal conductivity on the radial oscillation

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Analytical study of anisotropic compact star models

Cited by 89 publications

References 112 publications

Convection and cracking stability of spheres in general relativity

Convection and cracking stability of spheres in general relativity

Linear and Riccati equations in generating functions for stellar models in general relativity

Effect of viscosity and thermal conductivity on the radial oscillation and relaxation of relativistic stars

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