# Future Prospects for Constraining Nuclear Matter Parameters with Gravitational Waves

## TL;DR

This paper explores how future gravitational wave observations from neutron star mergers can better constrain nuclear matter parameters by analyzing correlations between tidal deformabilities and nuclear physics, considering multiple events and systematic errors.

## Contribution

It extends previous correlation analyses to varying chirp masses and proposes methods to improve nuclear parameter constraints using multiple detections and multidimensional correlations.

## Key findings

- Future GW observations can improve nuclear parameter bounds by ~30%.
- Systematic errors mainly stem from uncertainties in the equation of state.
- Multidimensional correlations can reduce systematic errors.

## Abstract

The gravitational wave emission from the merging binary neutron star system GW170817 arrived full of tidal information which can be used to probe the fundamental ultra-dense nuclear physics residing in these stars. In previous work, we used two-dimensional correlations between nuclear matter parameters and tidal deformabilities of neutron stars applying specifically to GW170817 to derive constraints on the former. Here, we extend this analysis by finding similar correlations for varying chirp masses, the dominant determining factor in the frequency evolution of the inspiral, such that one can apply the same method to future detections. We estimate how accurately one can measure nuclear parameters with future gravitational wave interferometers and show how such measurements can be improved by combining multiple events. We find that bounds on the nuclear parameters with future observations can improve from the current one with GW170817 only by $\sim 30\%$ due to the existence of systematic errors caused mainly by the remaining uncertainty in the equation of state near and just above the nuclear saturation density. We show that such systematic errors can be reduced by considering multidimensional correlations among nuclear parameters and tidal deformabilities with various neutron star masses.