We have presented the results of the analysis of 
maser spectral
features in ON2. We do not exclude the possibility that in some cases close
features in radial velocity are superimposed. They may flare consecutively,
leading to a drift in radial velocity. However, we do not exclude the
existence of real velocity variation of the features under the action of a
strong stellar wind or other influence coming for example from the
ultracompact HII region 
.
Anticorrelation in the flux of two features with similar radial velocity in
the ON2 maser is not a rare phenomenon. The anticorrelation was
consistent for some pairs of features, excluding only the period of maximum
activity in 1995. The different character of the anticorrelation for other
features may be due to the complex nature of this phenomenon.
The complicated character of the flux and radial velocity variations of maser features, the dependence between them (anticorrelation) and the radial velocity drift of an ensemble of features all show that these phenomena are
interrelated in ON2. The cause may be that the maser
is
located near (0.04 pc) to the ultracompact cometary HII region
(Hofner & Churchwell 1996) and follows its
action.
Acknowledgements
We would like to thank the associates of the Radio Astronomical Station of the Lebedev Physical Institute for generously providing observing time at the Pushchino RT-22 radio telescope and for their help during the observations and the Russian Foundation for Fundamental Research (Project Code 95-02-05087-a) for financial support. We also thank Dr. G.H. Macdonald for a number of comments which led to the improvement of the paper.