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The structure of a star's coronal magnetic field is a fundamental propertythat governs the high-energy emission from the hot coronal gas and the loss ofmass and angular momentum in the stellar wind. It is, however, extremelydifficult to measure. We report a new method to trace this structure inrapidly-rotating young convective stars, using the cool gas trapped on coronalfield lines as markers. This gas forms "slingshot prominences" which appear astransient absorption features in H-$\alpha$. By using different methods ofextrapolating this field from the surface measurements, we determine locationsfor prominence support and produce synthetic H-$\alpha$ stacked spectra. Theabsorption features produced with a potential field extrapolation match wellthis those observed, while those from a non-potential field do not. In systemswhere the rotation and magnetic axes are well aligned, up to $50\%$ of theprominence mass may transit the star and so produces a observable feature. Thisfraction may fall as low as $~2\%$ in very highly inclined systems. Ejectedprominences carry away mass and angular momentum at rates that vary by twoorders of magnitude, but which may approach those carried by the stellar wind.

Slingshot prominences: coronal structure, mass loss and spin down