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   71003
   Possibilities of heating processes of hot plasma in regions of
   formation of massive stars will be examined. We search for time
   variabilities up to scale of an week, which is 2 orders of magnitudes
   longer than e-folding times of flares of T Tauri stars. With a
   selection of a GMC, several cores are monitored at once, which enable
   efficient search for time variability. For the plasma heated by the
   reconnection of magnetic field similar to that found in T Tauri stars,
   variability should be found. For the plasma heated by the shock of
   stellar wind similar to that found in massive stars in main sequence,
   stationary emission is expected.
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