AI summary · arXiv: 2304.05100v1 · nucl-th

Investigating Dark Matter-Admixed Neutron Stars with NITR Equation of State in Light of PSR J0952-0607

Pinku Routaray, Sailesh Ranjan Mohanty, H. C. Das, Sayantan Ghosh, P. J. Kalita, V. Parmar, Bharat Kumar
Original paper Submitted to arXiv on 11 Apr. 2023 License: CC BY 4.0

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The essentials

  • Investigating properties of dark matter-admixed neutron stars using NITR model
  • Motivated by discovery of heaviest pulsar, PSR J0952-0607
  • NITR model developed based on extended relativistic mean field formalism
  • Validated for various finite nuclei and nuclear matter properties
  • Maximum mass and canonical radius consistent with PSR J0952-0607 and NICER limit
  • Two approaches used to obtain properties of dark matter-admixed neutron stars: non-gravitational and two-fluid models
  • Dark matter interactions lead to softer equation of state and reduced macroscopic properties
  • Observational data used to constrain amount of dark matter in neutron star without compromising stability or physical characteristics
  • Study expands on previous research on application of NITR model to dark matter-admixed neutron stars

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AI-generated keywords: Neutron Star Dark Matter NITR Model RMF Formalism Observational Data

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  • Original abstract
In this study, the authors investigate the properties of dark matter-admixed neutron stars using a new model called NITR (Naturalness-Inspired Two-Fluid Relativistic) equation of state (EOS). The motivation for this research comes from the recent discovery of the heaviest pulsar, PSR J0952-0607, in the disk of the Milky Way Galaxy. The pulsar has a mass of $2.35\pm0.17 \ M_\odot$, which is within the range predicted by the NITR model. The NITR model has been developed based on an extended relativistic mean field (RMF) formalism that takes into account the underlying symmetry arising in Quantum Chromodynamics (QCD) and solves the renormalization problem in conventional RMF theory. It has been validated by assessing its validity for various finite nuclei and nuclear matter properties, including incompressibility, symmetry energy, and slope parameter values. These values satisfy empirical/experimental limits currently available. Using the NITR model parameters, the authors calculate the maximum mass and canonical radius of a neutron star (NS), which are found to be consistent with both PSR J0952-0607 and the latest NICER limit. This confirms the reliability of the NITR model for predicting NS properties. To further test its consistency and validity, two approaches are employed to obtain properties of dark matter-admixed neutron stars: non-gravitational (single fluid) and two-fluid models. In both cases, interactions between dark matter particles only occur via gravity rather than with nucleons. The inclusion of dark matter interactions leads to a softer equation of state, resulting in reduced macroscopic properties such as maximum mass, radius, tidal deformability etc. Furthermore, observational data is used to constrain how much dark matter can be present within a neutron star. By comparing predictions from this study with various observational constraints obtained from different systems extensively calibrated using NITR model parameters; it aims to determine how much dark matter can be present in a neutron star without compromising its stability or other physical characteristics. Overall, this study expands on previous research by providing a more detailed analysis on application of NITR model to dark matter-admixed neutron stars and contributes to our understanding on their properties as well as insights into possible presence and effects of dark matter in these astrophysical objects.

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