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We use high time cadence, high spectral resolution optical observations todetect excess H-alpha emission from the 2 - 3 Myr old weak lined T Tauri starPTFO8-8695. This excess emission appears to move in velocity as expected if itwere produced by the suspected planetary companion to this young star. Theexcess emission is not always present, but when it is, the predicted velocitymotion is often observed. We have considered the possibility that the observedexcess emission is produced by stellar activity (flares), accretion from adisk, or a planetary companion; we find the planetary companion to be the mostlikely explanation. If this is the case, the strength of the H-alpha lineindicates 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 itsRoche lobe.

H-alpha Variability in PTFO8-8695 and the Possible Direct Detection of Emission from a 2 Million Year Old Evaporating Hot Jupiter