Relativistic gravitational collapse in noncomoving coordinates: The post-quasistatic approximation

Herrera, L.; Barreto, W.; Prisco, A. Di; Santos, N. O.

doi:10.1103/physrevd.65.104004

Cited by 48 publications

(74 citation statements)

References 70 publications

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“…Since we are going to follow closely the Misner approach [2] we shall use comoving coordinates (for a description of gravitational collapse in non-comoving coordinates, see [14] and references therein).…”

Section: The Energy-momentum Tensor and The Field Equationsmentioning

confidence: 99%

Dynamics of dissipative gravitational collapse

2004

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The Misner and Sharp approach to the study of gravitational collapse is extended to the dissipative case in, both, the streaming out and the diffusion approximations. The role of different terms in the dynamical equation are analyzed in detail. The dynamical equation is then coupled to a causal transport equation in the context of IsraelStewart theory. The decreasing of the inertial mass density of the fluid, by a factor which depends on its internal thermodynamics state, is reobtained, at any time scale. In accordance with the equivalence principle, the same decreasing factor is obtained for the gravitational force term. Prospective applications of this result to some astrophysical scenarios are discussed. *

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Section: The Energy-momentum Tensor and The Field Equationsmentioning

confidence: 99%

Dynamics of dissipative gravitational collapse

2004

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“…Therefore, the effective and physical variables share the same radial dependence. [35] Owing to the fact that (25a) involves only λ and ρ, it becomes…”

Section: Field Equations Effective Variables and The Post-quasistatimentioning

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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“…It is believed that large celestial systems are self-gravitating that are formed as a B M. Sharif msharif.math@pu.edu.pk R. Manzoor rubab.manzoor@umt.edu.pk 1 Department of Mathematics, University of the Punjab, Quaid-e-Azam Campus, Lahore 54590, Pakistan 2 Department of Mathematics, University of Management and Technology, Johar Town Campus, Lahore 54782, Pakistan consequence of gravitational collapse (Loveday et al 1996;Peacock et al 2001;Abazajian et al 2009). In this context, many researchers (Govender 1998;Govender et al 2001;Wagh et al 2001;Herrera et al 2002;Nogueira and Chan 2004;Macher et al 2005;Tewari 2006;Naidu et al 2006;Rajah and Maharaj 2008;Pinheiro and Chan 2008;Fayos and Torres 2008) explored characteristics of evolving selfgravitating systems in general relativity (GR). The evolution of self-gravitating system is usually described by a set of dynamical variables consisting of energy density, Weyl tensor, anisotropic pressures and kinematic variables (four acceleration, shear tensor as well as expansion parameter etc.…”

Section: Introductionmentioning

confidence: 98%

Structure scalars and cylindrical systems in Brans-Dicke gravity

Sharif

Manzoor

2015

Astrophys Space Sci

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This paper explores structure scalars of cylindrically symmetric spacetime in Brans-Dicke gravity. We construct twelve scalar factors using orthogonal splitting of the Reimann tensor and study their distinct dynamical interpretations. These structure scalars are used to derive a set of governing equations of the evolving system. It is concluded that cylindrical systems are necessarily inhomogeneous. Finally, we show that all possible static inhomogeneous cylindrical solutions can be obtained through structure scalars.

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Relativistic gravitational collapse in noncomoving coordinates: The post-quasistatic approximation

Cited by 48 publications

References 70 publications

Dynamics of dissipative gravitational collapse

Dynamics of dissipative gravitational collapse

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

Structure scalars and cylindrical systems in Brans-Dicke gravity

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