What do we learn about vector interactions from GW170817?

TL;DR

This paper investigates how vector-isovector meson interactions influence neutron star matter, using GW170817 data to compare different equations of state and their implications for neutron star properties.

Contribution

It provides a comparative analysis of three equations of state incorporating vector interactions, informed by recent gravitational wave and electromagnetic observations.

Findings

Different equations of state yield varying neutron star radii and masses.

Vector-isovector meson interactions significantly affect the symmetry energy and cooling processes.

GW170817 data constrains the properties of dense matter and the role of vector interactions.

Abstract

We analyze the role played by vector-isovector meson interaction in dense matter present in the interior of neutron stars in the light of new measurements made during the double neutron-star merger GW170817. These concern measurements of tidal deformability from gravitational waves and electromagnetic observations. Our study includes three different equations of state that contain different physical assumptions and matter compositions, namely the NL3 family, MBF, and CMF models. Other related quantities/relations analyzed are the neutron matter pressure, symmetry energy slope, stellar masses and radii, and Urca process threshold for stellar cooling.