The population of highly magnetized neutron stars

5th Compact Stars in the QCD Phase Diagram

Gomes, R.O.^1 ; Dexheimer, V.^2 ; Franzon, B.^3 ; Schramm, S.^3

Department of Astronomy, Universidade Federal Do Rio Grande Do sul, Porto Alegre, Brazil^1

Department of Physics, Kent State University, Kent

OH

44242, United States^2

FIAS, Ruth-Moufang 1, Frankfurt am Main

60438, Germany^3

关键词: Einstein-Maxwell equations;    Exotic particles;    Hadronic matters;    Magnetized neutron stars;    Poloidal magnetic field;    Relativistic mean fields;    Strong magnetic fields;    Zero temperatures;   

Others  :  https://iopscience.iop.org/article/10.1088/1742-6596/861/1/012016/pdf
DOI  :  10.1088/1742-6596/861/1/012016

来源: IOP

【 摘 要 】

In this work, we study the effects of strong magnetic field configurations on the population of neutron stars. The stellar matter is described within a relativistic mean field formalism which considers many-body force contributions in the scalar couplings. We choose the parametrization of the model that reproduces nuclear matter properties at saturation and also describes massive hyperon stars. Hadronic matter is modeled at zero temperature, in beta-equilibrium, charge neutral and populated by the baryonic octet, electrons and muons. Magnetic effects are taken into account in the structure of stars by the solution of the Einstein-Maxwell equations with the assumption of a poloidal magnetic field distribution. Our results show that magnetic neutron stars are populated essencialy by nucleons and leptons, due to the fact that strong magnetic fields decrease the central density of stars and, hence, supress the appearance of exotic particles.