Astronomy and Astrophysics – Astrophysics
Scientific paper
2005-12-12
Astrophys.J.640:L187-L190,2006
Astronomy and Astrophysics
Astrophysics
11 pages (aastex format), 2 figures submitted to ApJL
Scientific paper
10.1086/503419
Most, perhaps all, stars go through a phase of vigorous outflow during formation. We examine, through 3D MHD simulation, the effects of protostellar outflows on cluster formation. We find that the initial turbulence in the cluster-forming region is quickly replaced by motions generated by outflows. The protostellar outflow-driven turbulence (``protostellar turbulence'' for short) can keep the region close to a virial equilibrium long after the initial turbulence has decayed away. We argue that there exist two types of turbulence in star-forming clouds: a primordial (or ``interstellar'') turbulence and a protostellar turbulence, with the former transformed into the latter mostly in embedded clusters such as NGC 1333. Since the majority of stars are thought to form in clusters, an implication is that the stellar initial mass function is determined to a large extent by the stars themselves, through outflows which individually limit the mass accretion onto forming stars and collectively shape the environments (density structure and velocity field) in which most cluster members form. We speculate that massive cluster-forming clumps supported by protostellar turbulence gradually evolve towards a highly centrally condensed ``pivotal'' state, culminating in rapid formation of massive stars in the densest part through accretion.
Li Zhi-Yun
Nakamura Fumitaka
No associations
LandOfFree
Cluster Formation in Protostellar Outflow-Driven Turbulence does not yet have a rating. At this time, there are no reviews or comments for this scientific paper.
If you have personal experience with Cluster Formation in Protostellar Outflow-Driven Turbulence, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and Cluster Formation in Protostellar Outflow-Driven Turbulence will most certainly appreciate the feedback.
Profile ID: LFWR-SCP-O-501897