Neutron star crust and outer core equation of state from chiral effective field theory with quantified uncertainties

We study the order-by-order expansion of the energy per particle of asymmetric nuclear matter up to twice saturation density in chiral effective field theory (EFT) within a Bayesian framework. For this, we develop a two-dimensional Gaussian process (2D GP) that is trained using many-body perturbation theory results based on chiral two- and three-nucleon interactions from leading to next-to-next-to-next-to-leading order ( <a:math xmlns:a="http://www.w3.org/1998/Math/MathML"> <a:mrow> <a:msup> <a:mrow> <a:mi mathvariant="normal">N</a:mi> </a:mrow> <a:mn>3</a:mn> </a:msup> <a:mi>LO</a:mi> </a:mrow> </a:math> ). This allows for an efficient evaluation of the equation of state (EOS) and thermodynamic derivatives with EFT truncation uncertainties. After benchmarking our 2D GP against Bayesian uncertainties for pure neutron matter and symmetric matter, we study the energy per particle, pressure, and chemical potentials of neutron star matter in <c:math xmlns:c="http://www.w3.org/1998/Math/MathML"> <c:mi>β</c:mi> </c:math> equilibrium including EFT uncertainties. We investigate the phase diagram of neutron-rich matter from neutron- to proton-drip and to the uniform phase, including surface and Coulomb corrections. Based on this, we construct EOSs for the inner crust of neutron stars that are consistent with the chiral EFT results for uniform matter at <d:math xmlns:d="http://www.w3.org/1998/Math/MathML"> <d:mrow> <d:msup> <d:mrow> <d:mi mathvariant="normal">N</d:mi> </d:mrow> <d:mn>3</d:mn> </d:msup> <d:mi>LO</d:mi> </d:mrow> </d:math> .