Speaker
Ms
Chinatsu Watanabe
(Saitama University)
Description
Neutron stars are highly magnetized rotating compact stars. In 2010, a neutron star named PSR J1614-2230 has a mass of twice the solar mass (1.97$\pm$0.04M$\odot$). In 2013, a neutron star named PSR J0348+0432 with a mass of 2.01$\pm$0.04M$\odot$ was observed. Such massive neutron stars give strong constraints on the equation of state (EoS) of neutron star matter. In this study, we calculate radius of a neutron star using a perturbative prescription for various EoSs and relations of its total mass increased by magnetic fields. Also, we calculate the radius of the neutron star as a function of its total mass increased by rotation. As for the EoS, we use RMF theory. Moreover, we calculate mass-radius (MR) relation with both rotation and magnetic fields using 5 hadronic EoSs. We have the results of MR relation with both rotation and magnetic fields have the total mass of over twice the solar mass for all 5 hadronic EoSs.
Primary author
Ms
Chinatsu Watanabe
(Saitama University)
