Abstract
The number of discovered exoplanets now exceeds 1500, mostly due to the Kepler space instrument observations. Many of these planet orbit in less than a week around their host stars. This implies that the inward migration of those planets is a basic ingredient of successful theories of planet formation and evolution. Several mechanisms have been proposed to explain the observed periods, which lead to different orbit eccen- tricity and obliquity distributions. Here we summarise and discuss the results of obliqui- ties for two Kepler stars: HAT-P-7 and Kepler-25. These are interesting stellar systems as we could carry out a joint analysis using asteroseismology, transit lightcurve and the Rossiter-McLaughlin effect in order to measure the three dimensional obliquity.
Highlights
IntroductionHundreds of Jupiter-like planets with orbital periods of less than a week have been detected
Hundreds of Jupiter-like planets with orbital periods of less than a week have been detected. This indicates that an inward migration mechanism is required in theories of planet formation and evolution
The first one considers that planet migration occurs due to planet–disk interaction, which leads to circular orbits and orbital planes perpendicular to the stellar spin axis
Summary
Hundreds of Jupiter-like planets with orbital periods of less than a week have been detected. Measuring ψ is crucial, but requires a prior evaluation of the orbital inclination iorb and of the obliquity of the stellar spin-axis i , in addition to λ. The simplest technique uses the lightcurve modulation due to a spot at the surface of the star, combined with the rotational velocity of the star, v sin i in order to evaluate the stellar inclination [8]. This approach relies on at least two critical assumptions. This property has been widely used to infer the internal rotation rate of stars as well as the stellar inclination (e.g. 13; 14)
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