Neutron stars in a perturbative $f(R)$ gravity model with strong magnetic fields

Abstract

We investigate the effect of a strong magnetic field on the structure of neutron stars in a model with perturbative $f(R)$ gravity. The effect of an interior strong magnetic field of about $10^{17\sim 18}$ G on the equation of state is derived in the context of a quantum hadrodynamics (QHD) model. We solve the modified spherically symmetric hydrostatic equilibrium equations derived for a gravity model with $f(R)=R+\alpha R^2$. Effects of both the finite magnetic field and the modified gravity are detailed for various values of the magnetic field and the perturbation parameter $\alpha$ along with a discussion of their physical implications. We show that there exists a parameter space of the modified gravity and the magnetic field strength, in which even a soft equation of state can accommodate a large ($>2$ M${}_{\odot }$) maximum neutron star mass through the modified mass-radius relation.

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• Supermassive Neutron Stars in Axion $F(R)$ Gravity
• Modified Einstein's gravity as a possible missing link between sub- and super-Chandrasekhar type Ia supernovae
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• Logarithmic corrected Polynomial $f(R)$ inflation mimicking a cosmological constant
• GRMHD formulation of highly super-Chandrasekhar magnetized white dwarfs: stable configurations of non-spherical white dwarfs
• Thermodynamic topology of topological black hole in $F(R)$-ModMax gravity's rainbow
• Revisiting some physics issues related to the new mass limit for magnetized white dwarfs
• The Role of Baryon Structure in Neutron Stars
• Logarithmic corrected $F(R)$ gravity in the light of Planck 2015
• Equation of State of Neutron Stars with Junction Conditions in the Starobinsky Model
• Strong gravitational lensing by black hole in F(R) Euler Heisenberg Gravity's Rainbow
• Dipole magnetic field of neutron stars in $f(R)$ gravity
• Accelerating electrically charged ModMax black hole solutions in $F(R)$ gravity
• Bayesian Inference of Neutron Star Properties in $f(Q)$ Gravity Using NICER Observations