  We use high time cadence, high spectral resolution optical observations to
detect excess H-alpha emission from the 2 - 3 Myr old weak lined T Tauri star
PTFO8-8695. This excess emission appears to move in velocity as expected if it
were produced by the suspected planetary companion to this young star. The
excess emission is not always present, but when it is, the predicted velocity
motion is often observed. We have considered the possibility that the observed
excess emission is produced by stellar activity (flares), accretion from a
disk, or a planetary companion; we find the planetary companion to be the most
likely explanation. If this is the case, the strength of the H-alpha line
indicates that the emission comes from an extended volume around the planet,
likely fed by mass loss from the planet which is expected to be overflowing its
Roche lobe.

Earth and Planetary Astrophysics;Solar and Stellar Astrophysics