Fragmentation in Massive Star Formation

Abstract

Studies of evolved massive stars indicate that they form in a clustered mode. During the earliest evolutionary stages, these regions are embedded within their natal cores. Here, we show high-spatial-resolution interferometric dust continuum observations disentangling the cluster-like structure of a young massive star-forming region. The derived protocluster mass distribution is consistent with the stellar initial mass function. Thus, fragmentation of the initial massive cores may determine the initial mass function and the masses of the final stars. This implies that stars of all masses can form via accretion processes, and coalescence of intermediate-mass protostars appears not to be necessary.

5 pages text plus 2 figures

References in corpus (2)

• Multiple outflows in IRAS 19410+2336
• Hard X-ray emission from a young massive star-forming cluster

Cited by in corpus (50)

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