ASCA X-RAY-SPECTRA OF THE ACTIVE SINGLE STARS BETA-CETI AND PI(1)-URSAE-MAJORIS

We present X-ray spectra obtained by ASCA of two single, active stars, the G dwarf pi(1) UMa, and the G9/KO giant beta Cet. The spectra of both stars require the presence of at least two plasma components with different temperatures, 0.3-0.4 keV and similar to 0.7 keV, in order for acceptable fits to be obtained. The spectral resolving power and signal-to-noise ratio of the SIS spectra allow us to formally constrain the coronal abundances of a number of elements. In beta Cet, we find Mg to be overabundant, while other elements such as O, Ne, and N are underabundant, relative to the solar photospheric values. From the lower signal-to-noise ratio SIS spectrum of pi(1) UMa, we find evidence for underabundances of O, Ne, and Fe. These results are discussed in the context of the present understanding of elemental abundances in solar and stellar coronae.