Dr. Christian Schneider
X-rays and the hot side of star formation
The properties of planetary systems are set during the first few Myrs when the host star is still surrounded by its accretion disk. Matter flows through the disk onto the star, which requires powerful winds to remove excess angular momentum. X-ray observations allow us to study precisely these two phenomena. Accretion shocks emit mainly at X-ray wavelengths and the classical accretion tracers merely represent reprocessed X-rays. Similarly, protostellar jets can emit X-rays in their collimation zone, a phenomenon yet unexplained by theories. In this talk, I will present a new model for the accretion shock and a critical view on magnetic launching of protostellar jets inspired by X-ray and UV observations of young stellar systems.
Location: 31 Fitzwilliam Place, D02 XF86