Anisotropic ultra-compact object in Serrano–Liska gravity model

Abstract We implement a recent model proposed by Serrano–Liska (SL) (Alonso-Serrano and Liška, JHEP, 12:196, 2020) to study the ultra-compact star properties. The matter in interior is modeled quark model, deducted from QCD theory equipped with anisotropic pressure. Anisotropy used increase compactness of stars. intend see signature “quantum gravity” effect through SL was motivated quantum correction appearing black hole adding logarithmic term gravity entropy derive effective Einstein field equation. expect this also affects coupling constant $${\tilde{c}}$$ c ~ spherically symmetric metric yields terms $$\mathscr {O}({\tilde{c}})$$ O ( ) that can be expressed function $$\varXi (r)$$ Ξ r . vanishes at star’s exterior. found mass-radius relation prediction deviates one predicted standard Tolman–Oppenheimer–Volkoff (TOV) equation for $${\tilde{c}}\ge 10^7$$ ≥ 10 7 m $$^2$$ 2 have sufficiently deep enough potential produce quasi-normal mode. obtain echo frequency 15.2 kHz using maximum pressure contribution $${\tilde{c}}= = Because corresponding almost indistinguishable GR, value but not comparable result GW170817 data analysis, i.e., 72 Hz. To circumvent problem, we decrease increasing magnitude orders than On other hand, too large strength physically favored because learn case expected smaller Bekenstein term. Therefore, more precise gravitation measurements are crucial understand issue.