, and the
association of an X-ray source with a molecular cloud (Feigelson et al.
1993). The X-ray emission from the T Tauri stars is most likely due
to magnetic activity, similar to that observed in late type stars.
The X-ray emission from the molecular cloud is more difficult to
explain and may be due to shock heating of the gas by outflows from
the embedded young stars. In addition, X-rays have been detected from
the Orion nebula (Garmire et al. 1993). These X-rays are most likely
due to shocks in the outflows from the embedded stars. Such shocks can
also be responsible for producing nonthermal radio emission, as has been
observed in several regions of star formation (e.g., Anglada 1996).