---
author:
- Jérémy Leconte
- Gilles Chabrier
- Isabelle Baraffe
- Benjamin Levrard
bibliography:
- 'biblio.bib'
title: |
    Is tidal heating sufficient to explain bloated exoplanets?\
    Consistent calculations accounting for finite initial eccentricity
---

Introduction {#sec:intro}
============

Gravitational tides have marked out the history of science and astrophysics since the first assessment by Seleucus of Seleucia of the relation between the height of the tides and the position of the moon and the Sun in the second century BC. Modern astrophysics extended the study of gravitational tides in an impressive variety of contexts from the synchronization of the moon and other satellites to the evolution of close binary stars and even the disruption of galaxies.

The recent discoveries of short period extrasolar planetary systems and the determination of the anomalously large radius of some giant close-in exoplanets revived the need for a theory of planetary tides covering a wider variety of orbital configurations than previously encountered for the case of our own solar system planets. In particular, the orbital evolution of planetary systems such as HD 80606, with an orbital eccentricity of 0.9337 [@NLM01], and XO-3, with a stellar obliquity $\es\gtrsim37.3\pm3.7$ deg [@WJF09], cannot be properly treated with tidal 