### Speaker

### Description

In this work we investigate neutron stars (NS) in f (R, T ) gravity

for the case R + 2λT , R is the Ricci scalar, and T the trace of the

energy-momentum tensor. The hydrostatic equilibrium equations are

solved considering realistic equations of state (EOS). The NS masses

and radii obtained are subject to a joint constrain from massive pulsars

and the event GW170817. The parameter λ needs to be negative as in

previous NS studies, however, we found a minimum value for it due to the existence

of the NS crust. The pressure in this modified theory of gravity depends on the

inverse of the sound velocity. Since, this velocity is lower in the crust, |λ| needs to be very small. We found that the increment in the star mass is less

than 1%, much smaller than previous ones obtained not considering the

realistic stellar structure, and the star radius cannot become larger, its

changes compared to GR is less than 3.6% in all cases. The finding that

using several relativistic and non-relativistic models the variation on

the NS mass and radius is almost the same for all the EsoS, manifests

that our results are insensitive to the high-density part of the EOS.

It confirms that stellar mass and radii obtained in f(R,T) depends only on the NS crust, where the EoS is essentially the same for all the models. Finally, we highlight that our results indicate that conclusions obtained from NS studies

done in modified theories of gravity without using realistic EsoS that

describe correctly the NS interior can be unreliable.