REVIEW 2 cited by
Revisiting compact star in $F(R)$ gravity: Roles of chameleon potential and energy conditions
Not yet reviewed by Pith; the record is open.
This paper has not been read by Pith yet. Machine review is queued; the pith claim, tier, and objections will appear here once it completes.
SPECIMEN: schema-true, not a live event
T0 review · schema-true
One-sentence machine reading of the paper's core claim.
pith:XXXXXXXX · record.json · timestamp
Signed reviews
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.
Forward citations
Cited by 2 Pith papers
-
Rotating Fermion-Boson Stars in $R$-squared Gravity
R-squared gravity enlarges the equilibrium domain of rotating fermion-boson stars and raises static and Keplerian maximum masses relative to GR while remaining compatible with current compact-object constraints.
-
Radial oscillations of neutron stars in Starobinsky gravity and its Gauss-Bonnet extension
Radial oscillation frequencies of neutron stars are computed in Starobinsky and Gauss-Bonnet extended gravity, revealing a dynamical exterior and a low-density plateau in the fundamental mode.
Discussion (0). Continue with ORCID to comment.