The Radius Anomaly of Hot Jupiters: Linking Observations and Theory
Tuesday 3 July, 17:20
The discovery of the first transiting exoplanet HD209458b revealed an unexpectedly large radius that cannot be explained by standard evolution models. It has been shown that this anomaly stands for most of the hot Jupiters and different mechanisms have been proposed to explain their large radii. The most recognized theories either include energy transport to the interior or a slowing down of the cooling, leading to less contraction. While these mechanisms can explain the size of some inflated hot Jupiters, they cannot explain the whole population. To this date, more than 180 hot Jupiters have been detected which allows us to approach the problem within a statistical framework. We aim to quantify the fraction of energy needed to be transported to the interior (epsilon) to explain the observed radii of hot Jupiters. However, the observed parameters (radius, age, mass, ...) have uncertainties that can be significant. To remedy that, we develop a hierarchical probabilistic framework that allows us to incorporate these uncertainties and infer a distribution for epsilon. We benchmark our model to HD209458b and apply it to the sample of detected hot Jupiters.