  Parametric equations of state (EoSs) provide an important tool for
systematically studying EoS effects in neutron star merger simulations. In this
work, we perform a numerical validation of the M*-framework for parametrically
calculating finite-temperature EoS tables. The framework, introduced in Raithel
et 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 merger
with the SFHo finite-temperature EoS, as well as with the M*-approximation of
this same EoS, where the approximation uses the zero-temperature,
beta-equilibrium slice of SFHo and replaces the finite-temperature and
composition-dependent parts with the M*-model. We find that the approximate
version of the EoS is able to accurately recreate the temperature and thermal
pressure profiles of the binary neutron star remnant, when compared to the
results found using the full version of SFHo. We additionally find that the
merger dynamics and gravitational wave signals agree well between both cases,
with differences of ~1-2% introduced into the post-merger gravitational wave
peak frequencies by the approximations of the EoS. We conclude the M*-framework
can be reliably used to probe neutron star merger properties in numerical
simulations.
