  We present the analysis of the X-ray data of the young active star HD35850
obtained with ASCA and ROSAT. Our main goal was to see if there is a difference
in the elemental abundances of active stars between young and more evolved
objects. A two temperature plasma with subsolar abundances, of the order of Z =
0.15 - 0.3, is required to fit the SIS spectra. Similar results are obtained
from a ROSAT PSPC observation. Metal abundances of 0.2 - 0.4 the solar value
are required to fit both the ASCA and ROSAT data together. From a simultaneous
SIS0+SIS1 spectral fit, with 2T plasma models and abundances free to vary in
non-solar proportions, we find that, besides N, O and Ne for which we find very
low values, all other elements have values relative to solar abundances around
0.2-0.3. These subsolar abundances are in line with those typically observed in
more evolved, active stars like RS CVn and Algol-type binaries. The two
temperature values required to fit the ASCA SIS spectra are about 0.5 and 1.0
keV. These temperatures, especially the higher one, are lower with respect to
the values found for the RS CVn and Algol binaries or for the young star AB
Dor, but higher than other single G/K stars. All our data show that this
single, late F-type star is actually a very active source, indirectly
confirming that this fast rotating star is probably a young object. In the
simultaneous fit of the ASCA+ROSAT data, a third temperature is required.
However this is not just an addition of a softer component, but is more a
redistribution of the dominant temperatures. Indeed, the range spanned by the
three temperatures, from 5 to 15 million degrees, is not very large.
