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Title:
On the relative motions of dense cores and envelopes in star-forming molecular clouds
Authors:
Ayliffe, Ben A.; Langdon, James C.; Cohl, Howard S.; Bate, Matthew R.
Affiliation:
AA(School of Physics, University of Exeter, Stocker Road, Exeter EX4 4QL), AB(School of Physics, University of Exeter, Stocker Road, Exeter EX4 4QL), AC(School of Physics, University of Exeter, Stocker Road, Exeter EX4 4QL), AD(School of Physics, University of Exeter, Stocker Road, Exeter EX4 4QL)
Publication:
Monthly Notices of the Royal Astronomical Society, Volume 374, Issue 4, pp. 1198-1206. (MNRAS Homepage)
Publication Date:
02/2007
Origin:
MNRAS
Astronomy Keywords:
stars: formation, stars: kinematics, stars: low-mass, brown dwarfs, stars: luminosity function, mass function, ISM: clouds, ISM: kinematics and dynamics
DOI:
10.1111/j.1365-2966.2006.11259.x
Bibliographic Code:
2007MNRAS.374.1198A

Abstract

Hydrodynamical simulations of star formation indicate that the motions of protostars through their natal molecular clouds may be crucial in determining the properties of stars through competitive accretion and dynamical interactions. Walsh, Myers & Burton recently investigated whether such motions might be observable in the earliest stages of star formation by measuring the relative shifts of line-centre velocities of low- and high-density tracers of low-mass star-forming cores. They found very small (~0.1kms-1) relative motions. In this paper, we analyse the hydrodynamical simulation of Bate, Bonnell & Bromm and find that it also gives small relative velocities between high-density cores and low-density envelopes, despite the fact that competitive accretion and dynamical interactions occur between protostars in the simulation. Thus, the simulation is consistent with the observations in this respect. However, we also find some differences between the simulation and the observations. Overall, we find that the high-density gas has a higher velocity dispersion than that observed by Walsh et al. We explore this by examining the dependence of the gas velocity dispersion on density and its evolution with time during the simulation. We find that early in the simulation the gas velocity dispersion decreases monotonically with increasing density, while later in the simulation, when the dense cores have formed multiple objects, the velocity dispersion of the high-density gas increases. Thus, the simulation is in best agreement with the observations early on, before many objects have formed in each dense core.

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