Bulletin of the American Physical Society
5th Joint Meeting of the APS Division of Nuclear Physics and the Physical Society of Japan
Volume 63, Number 12
Tuesday–Saturday, October 23–27, 2018; Waikoloa, Hawaii
Session MF: Nuclear Matter and Nuclear Astrophysics
2:00 PM–5:00 PM,
Saturday, October 27, 2018
Hilton
Room: King's 2
Chair: Jeremy Holt, Texas A&M University
Abstract ID: BAPS.2018.HAW.MF.6
Abstract: MF.00006 : Magnetized rotational neutron stars and mass-radius relations
3:15 PM–3:30 PM
Presenter:
Chinatsu Watanabe
(Department of Physics, Saitama University)
Authors:
Chinatsu Watanabe
(Department of Physics, Saitama University)
Kota Yanase
(Department of Physics, Saitama University)
Naotaka Yoshinaga
(Department of Physics, Saitama University)
Ai Uehara
(Department of Physics, Saitama University)
Neutron stars are highly magnetized rotating compact stars.
It was reported in 2010 that a neutron star named PSR J1614-2230 making a binary system with a white dwarf has a mass of twice the solar mass (1.97±0.04M☉). In 2013, a neutron star named PSR J0348+0432 with a mass of 2.01±0.04M☉was observed. Such massive neutron stars give strong constraints on the equation of state (EoS) of neutron star matter.
In this study, we calculate mass, radius, and eccentricity of magnetized and deformed rotational neutron stars, using a perturbative prescription. As for the EoS a relativistic mean field approach is utilized. We obtain neutron star masses more than 2 M☉ from the mass-radius relation in a strong magnetic field.
To cite this abstract, use the following reference: http://meetings.aps.org/link/BAPS.2018.HAW.MF.6
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