The rotation of a star and the revolutions of its planets are not necessarily aligned. This
article reviews the measurement techniques, key findings, and theoretical interpretations …

We provide evidence that the obliquities of stars with close-in giant planets were initially
nearly random, and that the low obliquities that are often observed are a consequence of …

We carried out a Bayesian homogeneous determination of the orbital parameters of 231
transiting giant planets (TGPs) that are alone or have distant companions; we employed …

We determine the orbital eccentricities of individual small Kepler planets, through a
combination of asteroseismology and transit light-curve analysis. We are able to constrain …

I calculate the physical properties of 32 transiting extrasolar planet and brown-dwarf systems
from existing photometric observations and measured spectroscopic parameters. The …

We show that stars with transiting planets for which the stellar obliquity is large are
preferentially hot (T eff> 6250 K). This could explain why small obliquities were observed in …

In this paper we search for distant massive companions to known transiting gas giant
planets that may have influenced the dynamical evolution of these systems. We present new …

We measure the mass of a modestly irradiated giant planet, KOI-94d. We wish to determine
whether this planet, which is in a 22 day orbit and receives 2700 times as much incident flux …

Context. Several competing scenarios for planetary-system formation and evolution seek to
explain how hot Jupiters came to be so close to their parent stars. Most planetary …

Planet formation is generally described in terms of a system containing the host star and a
protoplanetary disk,–, of which the internal properties (for example, mass and metallicity) …