  We have studied the coronal X-ray emission of the recently discovered
short-period eclipsing binary HD 9770 with the BeppoSAX satellite. The data
from the Low Energy and Medium Energy Concentrator Spectrometers (LECS & MECS)
onboard BeppoSAX allow studying the spectrum of this star from 0.1 to 8 keV,
confirming that this is a very active coronal source, with strong flaring
activity. The X-ray emission most likely originates from the eclipsing binary
itself, rather than from the other visual component of the system. The X-ray
light curves could be modulated with the orbital period of the eclipsing
binary, with a hint for a different orbital modulation of the cooler and hotter
plasma. The X-ray spectrum is characterized by hot plasma, with the Fe K
complex at 6.7 keV clearly detected in the MECS spectrum, and it is well fitted
by a 2-temperature optically thin plasma model with low metal abundances ($\sim
0.3 Z_\odot$). These results are in line with those found for many other active
stars. As expected, during the flare the X-ray emission is dominated by hotter
plasma with a temperature $> 4$ keV. There is an indication that the metal
abundance may be somewhat higher during the flare.
