Minimal length, nuclear matter, and neutron stars

In this paper, we employ one variant of the Generalized Uncertainty Principle (GUP) model, i.e., Kempf-Mangano-Mann (KMM) and discuss impact GUP on EoS nuclear neutron star matter based Relativistic Mean Field (RMF) model. We input result in Serrano-Li\v{s}ka (SL) gravity theory to corresponding Neutron Star (NS) properties. have shown that upper bound for parameter from properties is $\beta \leq 2\times10^{-7}$ MeV$^{-2}$. If used $\beta$ calculate NS matter, considering SL $\tilde{c}$ as an independent parameter, found which modifies Einstein field equation, $\tilde{c} 10^7$ m$^2$. This beta determined by anisotropy magnitude smaller than pressure magnitude. By employing =2\times10^{-7}$ MeV$^{-2}$ = m$^2$, obtain mass-radius relation satisfies NICER data both PSR J0740+6620 (whose mass $\sim 2.1M_\odot$) J0030+0451 ($M\sim 1.4M_\odot$). Our perfectly matches constraint $^{87}$Rb cold-atom-recoil experiment. consider same strength additional logarithmic term entropy model are dependent, < MeV$^{-2}$, it clear lower > -16\times 10^{-34}$ The $10^{-40}$