Stellar Outflows in G333 GMC

Details Stellar Outflows in G333 GMC Stellar Outflows in G333 GMC

Apr 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006atnf.prop..270l&link_type=abstract

ATNF proposal M184, Semester: April, 2006

Other

Galactic, Mopra

Scientific paper

There are several star formation models competing to explain high mass star formation: the accretion, coalescence and turbulence models. A way in verifying these three models is through the study of stellar outflows. According to the accretion model, a highly collimated outflow should be observed. On the other hand the coalescence predicts a far less collimated outflow. The major problem with turbulence model is what are the driving forces in turbulence. With the study of outflow properties we can calculate how much kinetic energy is injected back into the interstellar medium, hence estimate the importance of stellar outflow in driving turbulence. The G333 Giant Molecular Complex contains sites of low and high mass star formation. We have selected seven possible outflow regions in this complex based on previous 13CO, C18O, CS and C34S transitions mapping and IR images from the Spitzer GLIMPSE programme. With the observation of high signal-to-noise CO line width, we can derive how much kinetic energy is injected back into the interstellar medium by outflow. We will also observe transition lines of CH3OH, CH3CN, HC3N and OCS to obtain further information of the outflows such as excitation temperature, gas temperature and outflow shocks.

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