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Relativistic stars in a cubic Galileon Universe

Research output: Contribution to journalArticle

Standard

Relativistic stars in a cubic Galileon Universe. / Ogawa, Hiromu; Kobayashi, Tsutomu; Koyama, Kazuya.

In: Physical Review D, Vol. 101, No. 2, 024026, 08.01.2020.

Research output: Contribution to journalArticle

Harvard

Ogawa, H, Kobayashi, T & Koyama, K 2020, 'Relativistic stars in a cubic Galileon Universe', Physical Review D, vol. 101, no. 2, 024026. https://doi.org/10.1103/PhysRevD.101.024026

APA

Ogawa, H., Kobayashi, T., & Koyama, K. (2020). Relativistic stars in a cubic Galileon Universe. Physical Review D, 101(2), [024026]. https://doi.org/10.1103/PhysRevD.101.024026

Vancouver

Ogawa H, Kobayashi T, Koyama K. Relativistic stars in a cubic Galileon Universe. Physical Review D. 2020 Jan 8;101(2). 024026. https://doi.org/10.1103/PhysRevD.101.024026

Author

Ogawa, Hiromu ; Kobayashi, Tsutomu ; Koyama, Kazuya. / Relativistic stars in a cubic Galileon Universe. In: Physical Review D. 2020 ; Vol. 101, No. 2.

Bibtex

@article{afd4cc0b0ecd41f0b21d9dcba351df89,
title = "Relativistic stars in a cubic Galileon Universe",
abstract = "We study relativistic stars in Hordenski theories that evade the gravitational wave constraints and exhibit the Vainshtein mechanism, focusing on a model based on the cubic Galileon Lagrangian. We derive the scalar field profile for static spherically symmetric objects in asymptotically de Sitter space-time with a linear time dependence. The exterior solution matches to the black hole solution found in the literature. Due to the Vainshtein mechanism, the stellar structure is indistinguishable from that of General Relativity with the same central density as long as the radius of the star is shorter than the Vainshtein radius. On the other hand, the scalar field is not suppressed beyond the Vainshtein radius. These solutions have an additional integration constant in addition to the mass of the star. ",
keywords = "gr-qc, astro-ph.CO, hep-th, RCUK, STFC, ST/N000668/1, ST/S000550/1",
author = "Hiromu Ogawa and Tsutomu Kobayashi and Kazuya Koyama",
year = "2020",
month = jan,
day = "8",
doi = "10.1103/PhysRevD.101.024026",
language = "English",
volume = "101",
journal = "Physical Review D",
issn = "1550-7998",
publisher = "American Institute of Physics Publising LLC",
number = "2",

}

RIS

TY - JOUR

T1 - Relativistic stars in a cubic Galileon Universe

AU - Ogawa, Hiromu

AU - Kobayashi, Tsutomu

AU - Koyama, Kazuya

PY - 2020/1/8

Y1 - 2020/1/8

N2 - We study relativistic stars in Hordenski theories that evade the gravitational wave constraints and exhibit the Vainshtein mechanism, focusing on a model based on the cubic Galileon Lagrangian. We derive the scalar field profile for static spherically symmetric objects in asymptotically de Sitter space-time with a linear time dependence. The exterior solution matches to the black hole solution found in the literature. Due to the Vainshtein mechanism, the stellar structure is indistinguishable from that of General Relativity with the same central density as long as the radius of the star is shorter than the Vainshtein radius. On the other hand, the scalar field is not suppressed beyond the Vainshtein radius. These solutions have an additional integration constant in addition to the mass of the star.

AB - We study relativistic stars in Hordenski theories that evade the gravitational wave constraints and exhibit the Vainshtein mechanism, focusing on a model based on the cubic Galileon Lagrangian. We derive the scalar field profile for static spherically symmetric objects in asymptotically de Sitter space-time with a linear time dependence. The exterior solution matches to the black hole solution found in the literature. Due to the Vainshtein mechanism, the stellar structure is indistinguishable from that of General Relativity with the same central density as long as the radius of the star is shorter than the Vainshtein radius. On the other hand, the scalar field is not suppressed beyond the Vainshtein radius. These solutions have an additional integration constant in addition to the mass of the star.

KW - gr-qc

KW - astro-ph.CO

KW - hep-th

KW - RCUK

KW - STFC

KW - ST/N000668/1

KW - ST/S000550/1

U2 - 10.1103/PhysRevD.101.024026

DO - 10.1103/PhysRevD.101.024026

M3 - Article

VL - 101

JO - Physical Review D

JF - Physical Review D

SN - 1550-7998

IS - 2

M1 - 024026

ER -

ID: 16981482