Magnetic Neutron Stars in f(R) gravity

Abstract

Neutron stars with strong magnetic fields are considered in the framework of f(R) gravity. In order to describe dense matter in magnetic field, the model with baryon octet interacting through $\sigma$$\rho$$\omega$-fields is used. The hyperonization process results in softening the equation of state (EoS) and in decreasing the maximal mass. We investigate the effect of strong magnetic field in models involving quadratic and cubic corrections in the Ricci scalar $R$ to the Hilbert-Einstein action. For large fields, the Mass-Radius relation differs considerably from that of General Relativity only for stars with masses close to the maximal one. Another interesting feature is the possible existence of more compact stable stars with extremely large magnetic fields ($\sim 6\times 10^{18}$ G instead of $\sim 4\times 10^{18}$ G as in General Relativity) in the central regions of the stars. Due to cubic terms, a significant increasing of the maximal mass is possible.

12 pages, 4 figures, 6 tables

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• Rotating Neutron Stars in F(R) Gravity with Axions
• Einstein's cluster mimicking compact star in the teleparallel equivalent of general relativity
• Traversable wormhole models in $f(R)$ gravity
• Decoupled Anisotropic Buchdahl's Relativistic Models in $f(\mathbb{R},\mathbb{T})$ Theory
• Neutron Stars in frames of $R^2$-gravity and Gravitational Waves
• Investigating dark energy by electromagnetic frequency shifts
• Constraining Quadratic $f(R)$ Gravity from Astrophysical Observations of the Pulsar J0704+6620
• Investigating dark energy by electromagnetic frequency shifts II: the Pantheon+ sample
• Modeling of non-rotating neutron stars in minimal dilatonic gravity
• Probing Strong Field $f(R)$ Gravity and Ultra-Dense Matter with the Structure and Thermal Evolution of Neutron Stars