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   62022
   ASCA and EUVE spectra of active late-type stars imply that Fe and other
   medium-Z elements may be 2-10 times less abundant in the coronae of
   these stars than in their photospheres (the MAD effect). These
   deficiencies may be related to the solar FIP effect, in which Fe and
   other low First Ionization Potential elements appear enriched in the
   solar corona over their photospheric values. The FIP effect is time
   variable. Here we request time with ASCA to measure the coronal
   abundances of the active K0-2 III star, 29 Dra, as a function of
   stellar longitude over its 31-day rotation cycle. Our goal is to learn
   whether the coronal abundances, and hence coronal magnetic structure,
   vary across the surface of 29 Dra in phase with the motion of dark
   starspots across the disk.
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