Neutron stars in a perturbative f(R) gravity model with strong magnetic fields
- Department of Physics, Soongsil University, Seoul 156-743 (Korea, Republic of)
- Department of Physics, Mimar Sinan Fine Arts University, Bomonti 34380, Istanbul (Turkey)
- İstanbul Technical University, Faculty of Science and Letters, Physics Engineering Department, Maslak 34469, Istanbul (Turkey)
- General Education Curriculum Center, Hanyang University, Seoul 133-791 (Korea, Republic of)
- National Astronomical Observatory of Japan, 2-21-1 Osawa, Mitaka, Tokyo 181-8588 (Japan)
In Kaluza-Klein electromagnetism it is natural to associate modified gravity with strong electromagnetic fields. Hence, in this paper we investigate the combined effects of a strong magnetic field and perturbative f(R) gravity on the structure of neutron stars. The effect of an interior strong magnetic field of about 10{sup 17−18} G on the equation of state is derived in the context of a quantum hadrodynamics (QHD) equation of state (EoS) including effects of the magnetic pressure and energy along with occupied Landau levels. Adopting a random orientation of interior field domains, we solve the modified spherically symmetric hydrostatic equilibrium equations derived for a gravity model with f(R) = R+αR{sup 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 α 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{sub s}un) maximum neutron star mass.
- OSTI ID:
- 22282633
- Journal Information:
- Journal of Cosmology and Astroparticle Physics, Vol. 2013, Issue 10; Other Information: Country of input: International Atomic Energy Agency (IAEA); ISSN 1475-7516
- Country of Publication:
- United States
- Language:
- English
Similar Records
A review on the relativistic effective field theory with parameterized couplings for nuclear matter and neutron stars
Neutron stars as laboratories for gravity physics