Speaker
Description
The detection of gravitational waves (GWs) from the binary neutron star (BNS) has opened a new window on the gravitational wave astronomy. With current sensitivities, detectable signals coming from compact objects like neutron stars turn out to be a crucial ingredient for probing their structure, composition, and evolution. Moreover, the astronomical observations on the pulsars and their mass-radius relations put important constraints on the dense matter equation of state (EoS). In this talk, we will consider a homogeneous and unpaired charge-neutral 3-flavor interacting quark matter with (m$^{4}$$_\text{s}$) corrections that account for the moderately heavy strange quark instead of the naive MIT bag model. In addition, we study a strange quark star in the context of recently proposed 4D Einstein-Gauss-Bonnet (EGB) theory of gravity. However, this theory is not well defined in four-dimensional spacetime. Thus, we thoroughly show that the equivalence of the actions in the regularized 4D EGB theory and in the original one is satisfied for a spherically symmetric spacetime. We pay particular attention to the possible existence of massive neutron stars of mass compatible with M ~ 2M$_\text{⨀}$. Our findings suggest that the fourth-order corrections parameter (a$_\text{4}$) of the QCD perturbation and coupling constant α of the GB term play an important role in the mass-radius relation as well as the stability of the quark star. Finally, we compare the results with the well-measured limits of the pulsars and their mass and radius extracted from the spectra of several X-ray compact sources.
