Abstract
In this work we study the effects of temperature on the equations of state obtained within a relativistic model, with and without $\ensuremath{\beta}$ equilibrium over a wide range of densities. We also compare the results of the equation of state, effective mass, and strangeness fraction for the TM1, NL3, and GL sets of parameters. We have checked that TM1 and NL3 are not appropriate for the description of neutron and protoneutron stars.
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