Relationship between the moment of inertia and the $k_2$ Love number of fluid extra-solar planets

TL;DR

This paper explores the relationship between the moment of inertia and the $k_2$ Love number in fluid exoplanets, providing analytical and semi-analytical models to help infer internal structures from future observations.

Contribution

It derives analytical and approximate relationships between the moment of inertia and $k_2$ for layered fluid exoplanets, including a practical rule of thumb for complex structures.

Findings

A unique N-$k_2$ relationship cannot be established.

A robust upper limit rule for N given $k_2$ is proposed.

The rule aligns with models of Jupiter and polytropic spheres.

Abstract

Context: Tidal and rotational deformation of fluid giant extra-solar planets may impact their transit light curves, making the $k_2$ Love number observable in the upcoming years. Studying the sensitivity of $k_2$ to mass concentration at depth is thus expected to provide new constraints on the internal structure of gaseous extra-solar planets. Aims: We investigate the link between the mean polar moment of inertia $N$ of a fluid, stably layered extra-solar planet and its $k_2$ Love number, aiming at obtaining analytical relationships valid, at least, for some particular ranges of the model parameters. We also seek a general, approximate relationship useful to constrain $N$ once observations of $k_2$ will become available. Methods: For two-layer fluid extra-solar planets, we explore the relationship between $N$ and $k_2$ by analytical methods, for particular values of the model parameters. We also explore approximate relationships valid over all the possible range of two-layer models. More complex planetary structures are investigated by the semi-analytical propagator technique. Results: A unique relationship between $N$ and $k_2$ cannot be established. However, our numerical experiments show that a `rule of thumb' can be inferred, valid for complex, randomly layered stable planetary structures. The rule robustly defines the upper limit to the values of $N$ for a given $k_2$, and agrees with analytical results for a polytrope of index one and with a realistic non-rotating model of the tidal equilibrium of Jupiter.