  Merging neutron stars are expected to produce hot, metastable remnants in
rapid differential rotation, which subsequently cool and evolve into rigidly
rotating neutron stars or collapse to black holes. Studying this metastable
phase and its further evolution is essential for the prediction and
interpretation of the electromagnetic, neutrino, and gravitational signals from
such a merger. In this work, we model binary neutron star merger remnants and
propose new rotation and thermal laws that describe post-merger remnants. Our
framework is capable to reproduce quasi-equilibrium configurations for generic
equations of state, rotation and temperature profiles, including nonbarotropic
ones. We demonstrate that our results are in agreement with numerical
relativity simulations concerning bulk remnant properties like the mass,
angular momentum, and the formation of a massive accretion disk. Because of the
low computational cost for our axisymmetric code compared to full
3+1-dimensional simulations, we can perform an extensive exploration of the
binary neutron star remnant parameter space studying several hundred thousand
configurations for different equation of states.
