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Parametric equations of state (EoSs) provide an important tool forsystematically studying EoS effects in neutron star merger simulations. In thiswork, we perform a numerical validation of the M*-framework for parametricallycalculating finite-temperature EoS tables. The framework, introduced in Raithelet al. (2019), provides a model for generically extending any cold,beta-equilibrium EoS to finite-temperatures and arbitrary electron fractions.In this work, we perform numerical evolutions of a binary neutron star mergerwith the SFHo finite-temperature EoS, as well as with the M*-approximation ofthis same EoS, where the approximation uses the zero-temperature,beta-equilibrium slice of SFHo and replaces the finite-temperature andcomposition-dependent parts with the M*-model. We find that the approximateversion of the EoS is able to accurately recreate the temperature and thermalpressure profiles of the binary neutron star remnant, when compared to theresults found using the full version of SFHo. We additionally find that themerger dynamics and gravitational wave signals agree well between both cases,with differences of ~1-2% introduced into the post-merger gravitational wavepeak frequencies by the approximations of the EoS. We conclude the M*-frameworkcan be reliably used to probe neutron star merger properties in numericalsimulations.

Finite-temperature effects in dynamical-spacetime binary neutron star merger simulations: Validation of the parametric approach