In addition to Kepler - 10b,
a second planet transiting the same star with a period of 45 days was sta - tistically validated, but the radial velocities were only good enough to set an upper limit of 20 Mearth for the mass of Kepler - 10c.
Not exact matches
Most importantly, the bolometric fluxes and angular radii reported here for a total of 498
planet host stars - with median accuracies of 1.7 % and 1.8 %, respectively - serve as a fundamental dataset to permit the re-determination of
transiting planet radii and masses with the Gaia
second data release to ~ 3 % and ~ 5 % accuracy, better than currently published precisions, and determined in an entirely empirical fashion.
On March 25, 2015, a team of astronomers using the Hubble Space Telescope revealed observations which indicate via the
transit method that Alpha Centauri B may have a
second planet «c» in a hot inner orbit, just outside
planet candidate «b.» After observing Alpha Centauri B in 2013 and 2014 for a total of 40 hours, the team failed to detect any
transits involving
planet b (previously detected using the radial velocity variations method and recently determined not to be observed edge - on in a
transit orbit around Star B).
The presence of a
second, non-transiting
planet was inferred from the
transit time variations (TTVs) of Kepler - 19b, over 8 quarters of Kepler photometry, although neither mas... ▽ More We report a detailed characterization of the Kepler - 19 system.
The presence of a
second, non-transiting
planet was inferred from the
transit time variations (TTVs) of Kepler - 19b, over 8 quarters of Kepler photometry, although neither mass nor period could be determined.
Second, we can learn how long the
planet's year is — since it only passes in front of the star once per orbit, the time between
transits is the
planet's year.