Neutron Star Mass Distribution in Binaries

11th Edoardo Amaldi Conference on Gravitational Waves

Lee, Chang-Hwan^1 ; Kim, Young-Min^1

Department of Physics, Pusan National University, Busan

46214, Korea, Republic of^1

关键词: Black holes;    Dwarf binaries;    Evolution process;    Mass distribution;    Neutron stars;   

Others  :  https://iopscience.iop.org/article/10.1088/1742-6596/716/1/012021/pdf
DOI  :  10.1088/1742-6596/716/1/012021

来源: IOP

【 摘 要 】

Massive neutron stars with ∼ 2M have been observed in neutron star-white dwarf binaries. On the other hand, well-measured neutron star masses in double-neutron-star binaries are still consistent with the limit of 1.5M. These observations raised questions on the neutron star equations of state and the neutron star binary evolution processes. In this presentation, a hypothesis of super-Eddington accretion and its implications are discussed. We argue that a 2M neutron star is an outcome of the super-Eddington accretion during the evolution of neutron star-white dwarf binary progenitors. We also suggest the possibility of the existence of new type of neutron star binary which consists of a typical neutron star and a massive compact companion (high-mass neutron star or black hole) with M ≥ 2M.