  The active late-type star AB Doradus was observed in February 1996 with the
Goddard High Resolution Spectrograph of the Hubble Space Telescope using the
low resolution G140L grating. The observations covered one half of the star's
rotation cycle (P = 0.514 d) with 11.5 min time resolution. The strong coronal
Fe XXI 1354.094 line formed at 10^7 K was analysed and its emission measure
(EM) derived. This EM is much higher than that derived from recent XMM-Newton
observations (Guedel et al. 2001), and earlier EXOSAT (Collier Cameron et al.
1988) and ASCA/EUVE (Mewe et al. 1996) data, as well, requiring a variability
by a factor of 5. The physical reason for the variability remains unknown,
since (outside flares) the observed broad band variability of AB Dor is much
smaller.
