Resolving kinematics in young stars

Classical T Tauri stars (CTTS) are surrounded by an accretion disk – the site of planet formation. Obviously, X-rays play a crucial role in the chemical evolution of the disk and thus planet formation. Furthermore, X-rays are established tracers of the hottest and fastest mass flows in CTTS system, potentially providing a handle on the elusive origin on the jet, its power and the angular momentum budget of accretion. CTTS emit X-rays from a variety of sources: Corona, accretion shock, jet outflow and possibly accreted mass accelerated upwards. Despite two
Chandra large programs we do not understand how each component contributes to the X-ray emission. To do so, we need to trace the kinematics of the hottest component in the system, i.e. we need to resolve the X-ray line profiles. The soft energy gratings on the X-ray surveyor offer
the only possible way to track the mass flows of the hot gas.