Regular Article - Theoretical Physics
Constraining properties of massive neutron star through R-mode
School of Physics and Optoelectronics, South China University of Technology, 510641, Guangzhou, People’s Republic of China
Accepted: 30 June 2022
Published online: 16 July 2022
Taking the GW190814 event as a clue, r-mode of 2.5 supermassive neutron star along with 1.4 canonical neutron star is investigated by using RNS code in the framework of rotating neutron star. Our conclusion further confirms that for the secondary star of GW190814, there exists a possibility that it is a rapid rotating supermassive neutron star in r-mode stable state. For super fast rotating neutron star with fixed spin frequency, the lower limit of its mass can be constrained by the critical spin frequency under r-mode. As the is EOS (equation of state) dependent, if the mass of neutron star with very high spin frequency can be observed in the future, the EOS of super-dense nuclear matter can be constrained by comparing the of different EOSs. At last, the effect of crust-core transition densities on r-modes of neutron stars is explored and discussed.
© The Author(s), under exclusive licence to Società Italiana di Fisica and Springer-Verlag GmbH Germany, part of Springer Nature 2022