Probing the Interiors of Very Hot Jupiters Using Transit Light Curves

TL;DR

This paper demonstrates that space-based photometry, especially from Kepler, can detect apsidal precession in very hot Jupiters, enabling constraints on their internal structure and core presence through transit light curve analysis.

Contribution

It introduces a method to measure planetary Love numbers via transit light curve variations caused by apsidal precession, focusing on very hot Jupiters with short orbital periods.

Findings

Apsidal precession dominates over relativistic and stellar quadrupole effects in very hot Jupiters.

Kepler can detect precession for planets with eccentricities as low as 0.003.

Transit shape changes are more informative than timing variations for interior characterization.

Abstract

Accurately understanding the interior structure of extra-solar planets is critical for inferring their formation and evolution. The internal density distribution of a planet has a direct effect on the star-planet orbit through the gravitational quadrupole field created by the rotational and tidal bulges. These quadrupoles induce apsidal precession that is proportional to the planetary Love number ($k_{2p}$, twice the apsidal motion constant), a bulk physical characteristic of the planet that depends on the internal density distribution, including the presence or absence of a massive solid core. We find that the quadrupole of the planetary tidal bulge is the dominant source of apsidal precession for very hot Jupiters ($a \lesssim 0.025$ AU), exceeding the effects of general relativity and the stellar quadrupole by more than an order of magnitude. For the shortest-period planets, the planetary interior induces precession of a few degrees per year. By investigating the full photometric signal of apsidal precession, we find that changes in transit shapes are much more important than transit timing variations. With its long baseline of ultra-precise photometry, the space-based \emph{Kepler} mission can realistically detect apsidal precession with the accuracy necessary to infer the presence or absence of a massive core in very hot Jupiters with orbital eccentricities as low as $e \simeq 0.003$. The signal due to $k_{2p}$ creates unique transit light curve variations that are generally not degenerate with other parameters or phenomena. We discuss the plausibility of measuring $k_{2p}$ in an effort to directly constrain the interior properties of extra-solar planets.