The presence of dark matter in neutron stars needs to be taken into account to match with observational data. In this work, we use IUFSU as EOS of NS and bosonic dark matter as EOS of dark matter core, respectively. We set mass of bosonic dark particles as 300 MeV and 400 MeV. The result of the moment of inertia of the NS that we obtain only reach lower limit of PSRJ037-3039A at M = 1.338M. Our calculations of dimensionless moment of inertia match with universal relations by Lattimer & Schutz [14] and Breu & Rezzolla [15]. We also shown crustal fraction of moment of inertia is compatible with the glitch phenomena in Vela pulsar.
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