An effective field theory approach to tidal dynamics of spinning astrophysical systems

TL;DR

This paper introduces an effective field theory framework to model tidal effects in astrophysical systems, applicable across Newtonian and relativistic regimes, with a focus on Newtonian objects like planets and stars.

Contribution

It develops a unified effective field theory approach to describe tidal dynamics, extending existing models with new corrections for deformations.

Findings

Derives dynamical equations for tidal interactions in the Newtonian regime.

Provides a systematic method to incorporate rotational and tidal deformations.

Connects effective field theory with classical tidal models.

Abstract

We develop a description of tidal effects in astrophysical systems using effective field theory techniques. While our approach is equally capable of describing objects in the Newtonian regime (e.g. moons, rocky planets, main sequence stars, etc.) as well as relativistic objects (e.g. neutron stars and black holes), in this paper we focus special attention on the Newtonian regime. In this limit, we recover the dynamical equations for the "weak friction model" with additional corrections due to tidal and rotational deformations.