Relativistic density functional theory for finite nuclei and neutron stars

TL;DR

This paper introduces relativistic density functional theory as a comprehensive framework for understanding the properties of finite nuclei and neutron stars, emphasizing the importance of Lorentz covariance in modeling dense, neutron-rich matter.

Contribution

It provides a pedagogical overview of applying relativistic density functional theory to neutron stars and discusses how laboratory experiments can constrain the equation of state of dense matter.

Findings

Relativistic density functional theory effectively models neutron star properties.

Laboratory experiments can significantly constrain the neutron-rich matter equation of state.

The framework incorporates Lorentz covariance essential for high-density regimes.

Abstract

The main goal of the present contribution is a pedagogical introduction to the fascinating world of neutron stars by relying on relativistic density functional theory. Density functional theory provides a powerful--and perhaps unique--framework for the calculation of both the properties of finite nuclei and neutron stars. Given the enormous densities that may be reached in the core of neutron stars, it is essential that such theoretical framework incorporates from the outset the basic principles of Lorentz covariance and special relativity. After a brief historical perspective, we present the necessary details required to compute the equation of state of dense, neutron-rich matter. As the equation of state is all that is needed to compute the structure of neutron stars, we discuss how nuclear physics--particularly certain kind of laboratory experiments--can provide significant constrains on the behavior of neutron-rich matter.