TY - JOUR

T1 - Neutron stars in f(R) gravity and scalar-tensor theories

AU - Kase, Ryotaro

AU - Tsujikawa, Shinji

N1 - Publisher Copyright:
Copyright © 2019, The Authors. All rights reserved.
Copyright:
Copyright 2020 Elsevier B.V., All rights reserved.

PY - 2019/6/21

Y1 - 2019/6/21

N2 - In f(R) gravity and Brans-Dicke theory with scalar potentials, we study the structure of neutron stars on a spherically symmetric and static background for two equations of state: SLy and FPS. In massless BD theory, the presence of a scalar coupling Q with matter works to change the star radius in comparison to General Relativity, while the maximum allowed mass of neutron stars is hardly modified for both SLy and FPS equations of state. In Brans-Dicke theory with the massive potential V (φ) = m2φ2/2, where m2 is a positive constant, we show the difficulty of realizing neutron star solutions with a stable field profile due to the existence of an exponentially growing mode outside the star. As in f(R) gravity with the R2 term, this property is related to the requirement of extra boundary conditions of the field at the surface of star. For the self-coupling potential V (φ) = λφ4/4, this problem can be circumvented by the field-dependent mass squared m2φ = 3λφ2 approaching 0 at spatial infinity. In this case, we numerically show the existence of neutron star solutions for both SLy and FPS equations of state and discuss how the mass-radius relation is modified as compared to General Relativity.

AB - In f(R) gravity and Brans-Dicke theory with scalar potentials, we study the structure of neutron stars on a spherically symmetric and static background for two equations of state: SLy and FPS. In massless BD theory, the presence of a scalar coupling Q with matter works to change the star radius in comparison to General Relativity, while the maximum allowed mass of neutron stars is hardly modified for both SLy and FPS equations of state. In Brans-Dicke theory with the massive potential V (φ) = m2φ2/2, where m2 is a positive constant, we show the difficulty of realizing neutron star solutions with a stable field profile due to the existence of an exponentially growing mode outside the star. As in f(R) gravity with the R2 term, this property is related to the requirement of extra boundary conditions of the field at the surface of star. For the self-coupling potential V (φ) = λφ4/4, this problem can be circumvented by the field-dependent mass squared m2φ = 3λφ2 approaching 0 at spatial infinity. In this case, we numerically show the existence of neutron star solutions for both SLy and FPS equations of state and discuss how the mass-radius relation is modified as compared to General Relativity.

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M3 - Article

AN - SCOPUS:85094064815

JO - Nuclear Physics A

JF - Nuclear Physics A

SN - 0375-9474

ER -