  We probe the relationship between surface magnetic fields and the X-ray
emitting corona in the rapidly rotating star AB Dor. Circularly polarised
spectra have been inverted to produce a surface (photospheric) magnetic field
map. This surface map has been extrapolated to model AB Dor's coronal field
topology and X-ray light curve. Chandra/LETG light curves of AB Dor from the
same epoch show intrinsic variability at the 30% level. Period analysis
indicates a fraction of this is due to rotational modulation. We measure
velocity shifts in emission line centroids as a function of rotation period and
find evidence of rotational modulation (max. vel. ~40+/- 13km/s). This
modulation may indicate the presence of a localised X-ray emitting region at
mid-to-high latitudes.
