Appearance of sexaquark in the core of neutron stars as a candidate of dark matter

Abstract

We study the appearance of sexaquark (uuddss) as a candidate of dark matter in the core of neutron stars while there has been no experimental evidence of this particle in laboratories so far. Regarding the observational constraints of supermassive pulsars as well as gravitational waves, we encounter a sexaquark dilemma for which we introduce a solution by quark deconfinement fulfilling all present constraints from multi-messenger astronomy, i.e., tidal deformability in accordance with GW170817 and maximum mass above the lower limit from PSR J0740+6620.

Exploring the Distribution and Impact of Bosonic Dark Matter in Neutron Stars

“…It is argued that high capture rates are more likely to happen toward the center of galaxies, where the density of DM is increasing [15][16][17]. Moreover, DM production inside NSs and supernova explosions can lead to large values of the DM fraction [5,6,18,19]. Among various models, a neutron decay anomaly by assuming a dark sector attracts considerable attention [20][21][22].…”

“…The impact of DM on NS properties has been investigated in various studies proposing a wide range of smoking guns [31][32][33][34][35][36][37]. Generally, the presence of DM can be considered through two scenarios: (i) a single-fluid object for which DM and BM interact also non-gravitationally via an EoS [18,19,[38][39][40][41][42], and (ii) two-fluid DM-admixed NSs where DM and BM are described by two EoSs and interact only by the gravitational force [10,[43][44][45][46][47][48][49]. For the former approach, DM is distributed throughout the whole NS, while for the latter, DM can form a dense core inside NSs or an extended halo around them.…”