TY - JOUR

T1 - Slowly rotating thin shell gravastars

AU - Uchikata, Nami

AU - Yoshida, Shijun

N1 - Publisher Copyright:
© 2016 IOP Publishing Ltd Printed in the UK.

PY - 2016/2/4

Y1 - 2016/2/4

N2 - We construct the solutions of slowly rotating gravastars with a thin shell. In the zero-rotation limit, we consider the gravastar composed of a de Sitter core, a thin shell, and Schwarzschild exterior spacetime. The rotational effects are treated as small axisymmetric and stationary perturbations. The perturbed internal and external spacetimes are matched with a uniformly rotating thin shell. We assume that the angular velocity of the thin shell, ω, is much smaller than the Keplerian frequency of the nonrotating gravastar, ωk. The solutions within an accuracy up to the second order of ω ωk are obtained. The thin shell matter is assumed to be described by a perfect fluid and to satisfy the dominant energy condition in the zero-rotation limit. In this study, we assume that the equation of state for perturbations is the same as that of the unperturbed solution. The spherically symmetric component of the energy density perturbations, δσ0, is assumed to vanish independently of the rotation rate. Based on these assumptions, we obtain many numerical solutions and investigate properties of the rotational corrections to the structure of the thin shell gravastar.

AB - We construct the solutions of slowly rotating gravastars with a thin shell. In the zero-rotation limit, we consider the gravastar composed of a de Sitter core, a thin shell, and Schwarzschild exterior spacetime. The rotational effects are treated as small axisymmetric and stationary perturbations. The perturbed internal and external spacetimes are matched with a uniformly rotating thin shell. We assume that the angular velocity of the thin shell, ω, is much smaller than the Keplerian frequency of the nonrotating gravastar, ωk. The solutions within an accuracy up to the second order of ω ωk are obtained. The thin shell matter is assumed to be described by a perfect fluid and to satisfy the dominant energy condition in the zero-rotation limit. In this study, we assume that the equation of state for perturbations is the same as that of the unperturbed solution. The spherically symmetric component of the energy density perturbations, δσ0, is assumed to vanish independently of the rotation rate. Based on these assumptions, we obtain many numerical solutions and investigate properties of the rotational corrections to the structure of the thin shell gravastar.

KW - gravastar

KW - perturbation

KW - rotation

KW - thin shell

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U2 - 10.1088/0264-9381/33/2/025005

DO - 10.1088/0264-9381/33/2/025005

M3 - Article

AN - SCOPUS:84952939955

VL - 33

JO - Classical and Quantum Gravity

JF - Classical and Quantum Gravity

SN - 0264-9381

IS - 2

M1 - 025005

ER -