EPJ Web of Conferences
Volume 11, 2011Detection and Dynamics of Transiting Exoplanets
|Number of page(s)||7|
|Section||Session 3: Atmospheres and interiors of exoplanets|
|Published online||16 February 2011|
Tidal instability in exoplanetary systems evolution
Institut de Recherche sur les Phenomenes Hors
Equilibre, UMR 6594, CNRS-Aix-Marseille University,
Marseille Cedex 13
2 Laboratoire d’Astrophysique de Marseille, UMR 6110, CNRS-Aix-Marseille University, 38 rue F. Joliot-Curie, Marseille
A new element is proposed to play a role in the evolution of extrasolar planetary systems: the tidal (or elliptical) instability. It comes from a parametric resonance and takes place in any rotating ﬂuid whose streamlines are (even slightly) elliptically deformed. Based on theoretical, experimental and numerical works, we estimate the growth rate of the instability for hot-jupiter systems, when the rotation period of the star is known. We present the physical process, its application to stars, and preliminary results obtained on a few dozen systems, summarized in the form of a stability diagram. Most of the systems are trapped in the so-called "forbidden zone", where the instability cannot grow. In some systems, the tidal instability is able to grow, at short timescales compared to the system evolution. Implications are discussed in the framework of misaligned transiting systems, as the rotational axis of the star would be unstable in systems where this elliptical instability grows.
© Owned by the authors, published by EDP Sciences, 2011
Current usage metrics show cumulative count of Article Views (full-text article views including HTML views, PDF and ePub downloads, according to the available data) and Abstracts Views on Vision4Press platform.
Data correspond to usage on the plateform after 2015. The current usage metrics is available 48-96 hours after online publication and is updated daily on week days.
Initial download of the metrics may take a while.