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The EUVE satellite spectrometers observed the prototype eclipsing binary Algol over nearly 1.5 orbital periods. Effective exposure times were 100 ksec and 89 ksec in the short wave (70-180 \AA) and medium wave (140-370 \AA) channels. High temperature (up to 20 MK) Fe XVI-XXIV emission lines are clearly detected in the overall spectrum. In addition, a quiescent continuum is present which increases towards shorter wavelengths. Using synthesized spectra of optically thin line and continuum emission folded through the instrumental response, we have examined constraints on the [Fe/H] coronal abundance in Algol. We find that the coronal Fe is underabundant by factors of $\approx$2--4 relative to solar photospheric values, unless an unreasonably large quantity of coronal plasma at T $>$ 30 MK is present in the quiescent spectrum. The latter possibility is, however, inconsistent with available X-ray data. Lightcurves of the high temperature EUV lines compared to line emission at He II 304 A show considerable differences, with much deeper minima present in the He II line during both primary and secondary eclipses. Toward the end of the observation a moderate flare lasting $\sim$6 hours was detected in the high temperature Fe emission lines.
This work was supported in part by NASA Contract NAS5-32492 and by the Lockheed Indepent Research Program.
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