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   63003
   We propose to perform a high signal-to-noise observation of the bright
   active binary VY Ari, a well known coronal source. VY Ari has recently
   been observed by the SAX instruments, and its ASCA observation will
   allow a comparison of the coronal parameters derived from ASCA and SAX
   observations. Also, given the superior spectral resolution of ASCA, the
   proposed observation will allow to determine the presence of eventual
   abundance ratio anomalies, which cannot be detected in the SAX
   observation but which could significantly influence the derived coronal
   parameters. The proposed observation will, in conjunction with the SAX
   observation, allow for a detailed and unprecedented study of the
   temperature structure and abundance in the corona of an active binary.
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