Eclipse mapping of the accretion stream in UZ Fornacis

We present a new method to map the surface brightness of the accretion stre ams in AM Herculis systems from observed light curves. Extensive tests of t he algorithm show that it reliably reproduces the intensity distribution of the stream for data with a signal-to-noise ratio greater than or similar t o 5. As a first application, we map the accretion stream emission of C IV l ambda 1550 in the polar UZ Fornacis using HST FOS high state spectra. We fi nd three main emission regions along the accretion stream: (1) On the balli stic part of the accretion stream, (2) on the magnetically funneled stream near the primary accretion spot, and (3) on the magnetically funneled strea m at a position above the stagnation region.