Obliquities of Exoplanet Host Stars from Precise Distances and Stellar Angular Diameters

Abstract

The next generation of exoplanet space photometry missions proposed by both NASA and ESA promise to discover small transiting planets around the nearest and brightest main-sequence stars. The physical and rotational properties of these stars, in conjunction with Gaia-precision distances, can be used to determine the inclination of the stellar rotation axis. Given edge-on orbital paths for transiting planets, stellar inclinations can be interpreted as obliquities projected into the line of sight, which can be used to more clearly reveal the system architectures of small planets and the factors that drive their orbital evolution. To demonstrate the method, we use a sample of simulated target stars for the NASA Transiting Exoplanet Survey Satellite (TESS) mission. Based on predicted characteristics of these stars and likely measurement uncertainties, we show that the expected TESS discoveries will allow us to finely differentiate the true underlying obliquity distribution. Under conservative assumptions in our illustrative example--in which the true distribution is assumed to contain systems drawn from both well-aligned and isotropic distributions (e.g., due to multiple migration channels)--the correct fractions can be determined to within $0.15$, thus enabling constraints on the evolutionary processes that shape system architectures. Moreover, because of the excellent astrometric precision expected from Gaia, this technique will also be applicable to the large number of planets already discovered by ${\textit Kepler}$ orbiting much more distant stars.