Interactions of flares comma accretion and wind in young stars

Young stars can produce Xrays by different mechanisms: Coronal activity,accretion shocks and shocks in outflows. We propose to observe two targetswithin one fieldofview (FOV): SU Aur is accreting mass from a disk and showsviolent coronal activity. We will study the time evolution of stellar flares ontime scales from seconds to minutes using the high count rate in the EPIC andthe OM to discover interactions with the accretion streams: The signature of theflare onset will differ in Xrays and UV between flares on coronal loops andflares on those field lines, which carry the accretion stream from the disk. ABAur is more massive, it shows a tentative modulation in the Xray luminosityapparently without spectral changes and contrary to model expectations. truncated!, Please see actual data for full text [truncated!, Please see actual data for full text]