Cold Supersonic Turbulence in Massive Cores

Details Cold Supersonic Turbulence in Massive Cores Cold Supersonic Turbulence in Massive Cores

May 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008aspc..387...38r&link_type=abstract

Massive Star Formation: Observations Confront Theory ASP Conference Series, Vol. 387, proceedings of the conference held 10-14 S

Astronomy and Astrophysics

Astronomy

3

Scientific paper

Cold massive cores are compared with their low-mass counterparts using a 3D radiative transfer code to model observational line profile data. We examine what can be learnt from different species and describe why HCN is a very unreliable infall tracer. A major difference between the two types of objects is that cold massive cores are much more turbulent than low-mass prestellar cores. We suggest that this highly supersonic turbulence is best understood as being due to a large population of clumps embedded in a more tenuous medium. Many of these clumps will eventually undergo gravitational collapse to form individual low-mass stars in a cluster around the massive stars.

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