Abstract
Tidal deformation of neutron star with multiquark core is calculated using nuclear and multiquark equations of state. The equation of state of the multiquark phase from the holographic Sakai-Sugimoto (SS) model is relatively stiff in the low density region and becomes softer at high densities. The values of Love number and dimensionless deformation parameter, k_{2} and Lambda , are found to be within the physically viable range under the present constraints. Radial pulsation frequencies of the multiquark core for n=0-5 modes are calculated for the entire mass range. For M_{mathrm{core}}simeq 2 M_{odot }, the fundamental-mode frequency is approximately 2.5 kHz for the energy density scale epsilon _{s}=23.2037 GeV/fm^{3} of the holographic SS model, this frequency is proportional to sqrt{epsilon _{s}}.
Highlights
A number of detections of massive neutron stars (NS) with masses approximately larger than 2 solar mass (M ) [1– 12] indicates that the equation of state (EoS) of the core of the massive NS could be softer than the usual stiff baryonic nuclear matter in the crust
We found that for massive NS with multiquark core, the values of deformation parameters are within the allowed constraints from LIGO/Virgo
6 Conclusions and discussions The deformation parameters of the NS with multiquark core and multiquark star (MQS) have been calculated in the holographic SS model
Summary
A number of detections of massive neutron stars (NS) with masses approximately larger than 2 solar mass (M ) [1– 12] indicates that the equation of state (EoS) of the core of the massive NS could be softer than the usual stiff baryonic nuclear matter in the crust. Substantial scan of various forms of the EoS based on the sound speed and adiabatic index reveals the possibility that the massive NS has a quark matter core [13]. With the prospect of massive NS above 2M containing quark matter core from observations, it is interesting to investigate how the holographic multiquark EoS fit into the observational constraints. 4. Tidal deformabilities and other properties such as moment of inertia, sound speed and EoS of hybrid stars in holographic models of quark and nuclear matter are calculated in Refs. In this work we calculate the Love number k2 and of the NS with multiquark core by adapting Chiral Effective Field Theory (CET) EoS [37] and FYSS EoS [38–40] for the nuclear crust. 3. The tidal deformation of the NS with multiquark core and MQS are calculated in Sect.
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