Imaging the outflow of 2 MK gas from the Orion Nebula

Details Imaging the outflow of 2 MK gas from the Orion Nebula Imaging the outflow of 2 MK gas from the Orion Nebula

Oct 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008xmm..prop..162b&link_type=abstract

XMM-Newton Proposal ID #06059001

Computer Science

Supernovae, Supernova Remnants, Diffuse (Galactic) Emission And Isolated Neutron Stars, Orion Nebula Sw

Scientific paper

Our discovery of diffuse X-ray emission in the Orion Nebula has demonstrated that hot bubbles, created by shocks in the powerful, hypersonic winds of high- mass stars, are a common feature of high-mass star-forming regions, not only those that host many early O-type stars. Pressure equilibrium with the HII gas and an apparent stream of 1.8 MeV emission, caused by the radioactive decay of 26Al, connecting the Nebula region to the nearby Eridanus Superbubble suggest the hot gas is not confined. The outflow of hot gas from such regions could provide a continual source of enrichment of the ISM, complementary to the discrete but rare input of supernovae. Our aim is to directly image the outflow of X-ray-emitting hot gas from the Orion Nebula.

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