Minimal Length, Nuclear Matter, and Neutron Stars

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In this paper, we employ one variant of the Generalized Uncertainty Principle (GUP) model, i.e., the Kempf-Mangano-Mann (KMM) model, and discuss the impact of GUP on the EoS of nuclear and neutron star matter based on the Relativistic Mean Field (RMF) model.

• We input the result in the Serrano-Li\v{s}ka (SL) gravity theory to discuss the corresponding Neutron Star (NS) properties.
• We have shown that the upper bound for the GUP parameter from nuclear matter properties is $\beta \leq 2\times10^{-7}$ MeV$^{-2}$.
• If we used this $\beta$ upper bound to calculate NS matter, and considering SL parameter $\tilde{c}$ as an independent parameter, we have found that the upper bound for the SL parameter, which modifies the Einstein field equation, is $\tilde{c} \leq 10^7$ m$^2$.