# XQCD 2019 (The 17th International Conference on QCD in Extreme Conditions)

24-26 June 2019
Bunkyo School Building, Tokyo Campus, University of Tsukuba
Japan timezone

## Rotating neutron star in strong magnetic fields and the MR relations

24 Jun 2019, 12:15
25m
134 (Bunkyo School Building, Tokyo Campus, University of Tsukuba)

### 134

#### Bunkyo School Building, Tokyo Campus, University of Tsukuba

3-29-1 Otsuka Bunkyo-ku Tokyo 112-0012 Japan
Oral talk

### 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)

 Slides