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7. Summary and conclusion
Our simultaneous optical/X-ray observations verify CN Leo’s
status as a star of intermediate activity. Compared to earlier
Mdwarfs, its X-ray luminosity is lower, its coronal temperatures
is dominated by cooler components, and the abundances lack
a pronounced inverse FIP effect. CN Leo exhibits three different
“quasi-quiescent” levels in X-rays during the observations,
which are also clearly observed in the chromospheric lines in the
optical. While the highest of these states on December 11th 2005
may be due to the tail of the decay phase of a long duration flare,
there is no such obvious explanation for the higher activity state
on December 13th compared to the May 2004 observation. Since
the X-ray flux in the 2004 observation is comparable to the lowest
X-ray luminosity measured by ROSAT, we regard this state
as the true quasi-quiescent level of CN Leo.
We find coronal densities from the Ovii triplets ne ∼
1010 cm−3, while the Ne ix measurements are consistent with
the low-density limit. During the flare on the second night, we
also measured transition region densities from two He ii lines
that also give ne ∼ 1010 cm−3.