Revisiting compact star in $F(R)$ gravity: Roles of chameleon potential and energy conditions

Abstract

We reexamine the static and spherical symmetric compact star configuration in the $R^2$ model of the $F(R)$ gravity theory. With asymptotic solutions for the additional scalar degrees of freedom, we refine analysis on the external geometry and settle the scalar-hair problem argued in previous works. Performing the numerical integration of the modified Tolman-Oppenheimer-Volkoff equations as a two-boundaries-value problem, we further discuss the scalar-field distribution inside the compact stars and its influence on the mass-radius relation. We show that the chameleon potential plays an essential role in determining the scalar-field profile inside the star. The scalar field often behaves as a quintessential field that effectively decreases the mass of compact stars with lower central energy density.

37 pages, 22 figures, 1 table. Version to appear in PRD

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Cited by in corpus (8)

• Compact stars in Rastall gravity: hydrostatic equilibrium and radial pulsations
• Neutron Star in Covariant $f(Q)$ gravity
• Moment of inertia and compactness of quark stars within the context of $f(R,T,L_m)$ gravity
• Compact star in noninteger power model of $f(R)$ gravity
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• Scalaron dark matter and the thermal history of the universe
• Unveiling a universal relationship between the f(R) parameter and neutron star properties
• Thermodynamics, Phase Transitions, and Geodesic Structure of F(R)-Phantom Banados-Teitelboim-Zanelli (BTZ) Black Holes