On Magnetized Neutron Stars
arXiv:1411.7209 · doi:10.1088/1475-7516/2015/08/002
Abstract
In this work we review the formalism normally used in the literature about the effects of density-dependent magnetic fields on the properties of neutron and quark stars, expose some ambiguities that arise and propose a way to solve the related problem. Our approach explores more deeply the concept of pressure, yielding the so called chaotic magnetic field formalism for the stress tensor. We also use a different way of introducing a variable magnetic field, which depends on the energy density rather than on the baryonic density, which allows us to build a parameter free model.
6 Figures + Appendix. Final version to match the published one
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- Role of vector channel in different classes of (non) magnetized neutron stars
- Gravitational Wave Signatures of Highly Magnetized Neutron Stars
- Quark matter under strong magnetic fields
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- Hyperon threshold and stellar radii
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- Antikaon condensation in magnetized neutron star matter within the framework of the -cut scheme
- Charged scalar boson in Melvin universe