Abstract
In this work we study the effects of temperature on the equations of state obtained within a relativistic model with and without β equilibrium, over a wide range of densities. We integrate the TOV equations. We also compare the results of the equation of state, effective mass and strangeness fraction for the TM1, NL3 and GL sets of parameters, as well as investigating the importance of antiparticles in the treatment. We have checked that TM1 and NL3 are not appropriate for the description of neutron and protoneutron stars.
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