2014/05/26 by Artyom V. Astashenok, Salvatore Capozziello, Sergei D. Odintsov · 2 citations
Physics and Astronomy · #Baryon #Black Holes and Theoretical Physics #Cosmology #Cosmology and Gravitation Theories #Equation of state #General relativity #Magnetic field #Neutron star #Pulsars and Gravitational Waves Research #Stars #Theory of relativity #astro-ph.HE #f(R) gravity #gr-qc #hep-th
paper · pdf · doi:10.1007/s10509-014-2182-6
12 pages, 4 figures, 6 tables
arxiv created 2014/05/26 · openalex publication_date 2014/12/01 · arxiv updated 2015/06/19 · openalex created_date 2016/06/24 · openalex updated_date 2026/08/05
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 σρω-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 (∼ 6× 1018 G instead of ∼ 4× 1018 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.