# Bayesian modeling of the nuclear equation of state for neutron star tidal deformabilities and GW170817

## TL;DR

This paper uses Bayesian methods with nuclear physics data to predict neutron star tidal deformabilities and explore their relation to nuclear properties, assuming no phase transitions at high density.

## Contribution

It introduces a Bayesian framework combining nuclear theory and experimental data to model the neutron star equation of state and predict tidal deformabilities.

## Key findings

- Predicted neutron star tidal deformabilities consistent with GW170817 observations.
- Established correlations between tidal deformability and finite nuclear properties.
- Provided mass-radius relations based on the Bayesian equation of state.

## Abstract

We present predictions for neutron star tidal deformabilities obtained from a Bayesian analysis of the nuclear equation of state, assuming a minimal model at high-density that neglects the possibility of phase transitions. The Bayesian posterior probability distribution is constructed from priors obtained from microscopic many-body theory based on realistic two- and three-body nuclear forces, while the likelihood functions incorporate empirical information about the equation of state from nuclear experiments. The neutron star crust equation of state is constructed from the liquid drop model, and the core-crust transition density is found by comparing the energy per baryon in inhomogeneous matter and uniform nuclear matter. From the cold $\beta$-equilibrated neutron star equation of state, we then compute neutron star tidal deformabilities as well as the mass-radius relationship. Finally, we investigate correlations between the neutron star tidal deformability and properties of finite nuclei.