Title:

	Stellar Coronae in Young Solar Type Stars



Gaitee Hussain
ESO



Abstract:

Coronal magnetic fields in young solar-type (G and K-type)
stars are the key mechanism by which many fundamental
processes occur in young stars and their surrounding
systems. For instance, the angular momentum evolution of
young stars is explained by the interaction of coronal
magnetic fields with their surrounding disks, and large
flares originating in stellar coronae are likely to be
responsible for seeding the protoplanetary disks in T Tauri
stars. By combining Chandra X-ray observations and surface
magnetic field maps obtained using the technique of Zeeman
Doppler imaging, we can build and test realistic
three-dimensional models of young cool stars for the first
time. Recent results suggest that the large scale structure
of the corona changes quickly as T Tauri stars approach the
main sequence. I will discuss these latest results and
outline the implications that this has for the efficiency
with which disk braking can occur.