Paper:	Non-Thermal Emission from Massive Young Stellar Objects
Volume:	422, High Energy Phenomena in Massive Stars
Page:	122
Authors:	Parkin, E. R.; Pittard, J. M.; Hoare, M. G.
Abstract:	In the young stellar object (YSO) phase of their lives, massive stars drive bipolar molecular outflows. These outflows produce beautiful, often hourglass shaped, cavities. The central star possesses a powerful stellar wind ( v ∼ 2000 kms-1), and possibly a dense equatorial disk wind ( v ∼ 400 kms-1), which collide with the inner surface of the bipolar cavity and produces hot ( T ∼ 105 – 108 K) shocked plasma. A reverse shock is formed at the point where the ram pressure between the preshock flow balances the thermal pressure of the postshock flow and provides a site for the acceleration of non-thermal particles to relativistic energies. Hydrodynamical models of the wind interaction, coupled with calculations of the non-thermal energy spectrum, are used to explore the observable synchrotron and gamma-ray emission from these objects.

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