  The nearby (d=5.0 pc) brown dwarf LP944-20 was observed with the XMM-Newton
satellite on 07 January 2001. The target was detected with the Optical Monitor
(V=16.736$\pm$0.081), but it was not detected during the $\approx 48$ ks
observation with the X-ray telescopes. We determine a $3\sigma$ upper limit for
the X-ray emission from this object of $L_{X}<3.1 \times 10^{23}$ $ergs \cdot
s^{-1}$, equivalent to a luminosity ratio upper limit of $\log{(L_{X}/L_{bol})}
\le -6.28$. This measurement improves by a factor of 3 the previous
\emph{Chandra} limit on the quiescent X-ray flux. This is the most sensitive
limit ever obtained on the quiescent X-ray emission of a brown dwarf. Combining
the XMM data with previous \emph{ROSAT} and \emph{Chandra} data, we derive
flare duty cycles as a function of their luminosities. We find that very strong
flares [Log$(L_X/L_{bol})>-$2.5] are very rare (less than 0.7% of the time).
Flares like the one detected by Chandra [Log$(L_X/L_{bol})=-$4.1] have a duty
cycle of about 6%, which is lower than the radio flare duty cycle ($\sim$13%).
When compared with other M dwarfs, LP944-20 appears to be rather inactive in
X-rays despite of its relative youth, fast rotation and its moderately strong
activity at radio wavelengths.
