Chin. Phys. Lett.  2019, Vol. 36 Issue (4): 049701    DOI: 10.1088/0256-307X/36/4/049701
Neutrino Emission and Cooling of Dark-Matter-Admixed Neutron Stars
Wen-Bo Ding1**, Zi Yu2, Yan Xu3, Chun-Jian Liu1, Tmurbagan Bao4
1College of Mathematics and Physics, Bohai University, Jinzhou 121000
2College of Science, Nanjing Forestry University, Nanjing 210037
3Changchun Observatory, National Astronomical Observatories, Chinese Academy of Sciences, Changchun 130117
4College of Physics And Electronic Information, Inner Mongolia University for the Nationalities, Tongliao 028043
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Wen-Bo Ding, Zi Yu, Yan Xu et al  2019 Chin. Phys. Lett. 36 049701
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Abstract The GW170817 binary neutron star merger event in 2017 has raised great interest in the theoretical research f neutron stars. The structure and cooling properties of dark-matter-admixed neutron stars are studied here using relativistic mean field theory and cooling theories. The non-self-annihilating dark matter (DM) component is assumed to be ideal fermions, among which the weak interaction is considered. The results show that pulsars J1614-2230, J0348+0432 and EXO 0748-676 may all contain DM with the particle mass of 0.2–0.4 GeV. However, it is found that the effect of DM on neutron star cooling is complicated. Light DM particles favor the fast cooling of neutron stars, and the case is converse for middle massive DM. However, high massive DM particles, around 1.0 GeV, make the low mass (around solar mass) neutron star still undergo direct Urca process of nucleons at the core, which leads the DM-admixed stars cool much more quickly than the normal neutron star, and cannot support the direct Urca process with a mass lower than 1.1 times solar mass. Thus, we may conjecture that if small (around solar mass) and super cold (at least surface temperature 5–10 times lower than that of the usual observed data) pulsars are observed, then the star may contain fermionic DM with weak self-interaction.
Received: 26 December 2018      Published: 23 March 2019
PACS:  97.60.Jd (Neutron stars)  
  95.30.Cq (Elementary particle processes)  
  26.60.Dd (Neutron star core)  
  26.60.Kp (Equations of state of neutron-star matter)  
Fund: Supported by the National Natural Science Foundation of China under Grant Nos 11805022, 11265009, 11175077 and 11271055, and the Youth Innovation Promotion Association of the Chinese Academy of Sciences under Grant No 2016056.
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Wen-Bo Ding
Zi Yu
Yan Xu
Chun-Jian Liu
Tmurbagan Bao
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