Abstract
The dynamical evolution of planetary systems, after the evaporation of the accretion disk, is the result of the competition between tidal dissipation and the net angular momentum loss of the system. The description of the diversity of orbital configurations, and correlations between parameters of the observed system (e.g. in the case of hot jupiters), is still limited by our understanding of the transport of angular momentum within the stars, and its effective loss by magnetic braking. After discussing the challenges of modelling tidal evolution for exoplanets, I will review recent results showing the importance of tidal interactions to test models of planetary formation. This kind of studies rely on the determination of stellar radii, masses and ages. Major advances will thus be obtained with the results of the PLATO 2.0 mission, selected as the next M-class mission of ESA’s Cosmic Vision plan, that will allow the complete characterisation of host stars using asteroseismology.
Highlights
Unlike our own solar system, many extrasolar systems have planets orbiting very close to their stars, with orbital periods not greater than about ten days
It is generally admitted that the convective zone of late-type stars host a hydromagnetic dynamo at the origin of their magnetic activity, which is in turn responsible for the angular momentum loss (AML)
In any case magnetic braking in return has an effect on the dynamical evolution of the system because the tidal torque is a function of the difference between the orbital period and the stellar rotational period
Summary
Unlike our own solar system, many extrasolar systems have planets orbiting very close to their stars, with orbital periods not greater than about ten days For those planets, the typical distance to the star is less than 0.1 AU and interactions with the host through radiation, magnetism or tides may be significant. It is generally admitted that the convective zone of late-type stars host a hydromagnetic dynamo at the origin of their magnetic activity, which is in turn responsible for the angular momentum loss (AML). This is generally explained by magnetic braking, where a wind of charged particles can efficiently extract angular momentum from the star with a very low mass loss rate.
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