Finite-temperature expansion of the dense-matter equation of state

Abstract

In this work we provide a new, well-controlled expansion of the equation of state of dense matter from zero to finite temperatures (T), while covering a wide range of charge fractions (YQ), from pure neutron to isospin symmetric nuclear matter. Our expansion can be used to describe neutron star mergers and core-collapse supernova explosions using as a starting point neutron star observations, while maintaining agreement with laboratory data, in a model independent way. We suggest new thermodynamic quantities of interest that can be calculated from theoretical models or directly inferred by experimental data that can help constrain the finite T equation of state. With our new method, we can quantify the uncertainty in our finite T and YQ expansions in a well-controlled manner without making assumptions about the underlying degrees of freedom. We can reproduce results from a microscopic equation of state up to T=100 MeV for baryon chemical potential μB≳1100 MeV (∼1−2 nsat) within 5% error, with even better results for larger μB and/or lower T. We investigate the sources of numerical and theoretical uncertainty and discuss future directions of study.

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