Induced Core Formation Time in Subcritical Magnetic Clouds by Large-Scale Trans-Alfvénic Flows

Abstract

We clarify the mechanism of accelerated core formation by large-scale nonlinear flows in subcritical magnetic clouds by finding a semi-analytical formula for the core formation time and describing the physical processes that lead to them. Recent numerical simulations show that nonlinear flows induce rapid ambipolar diffusion that leads to localized supercritical regions that can collapse. Here, we employ non-ideal magnetohydrodynamic simulations including ambipolar diffusion for gravitationally stratified sheets threaded by vertical magnetic fields. One of the horizontal dimensions is eliminated, resulting in a simpler two-dimensional simulation that can clarify the basic process of accelerated core formation. A parameter study of simulations shows that the core formation time is inversely proportional to the square of the flow speed when the flow speed is greater than the Alfvén speed. We find a semi-analytical formula that explains this numerical result. The formula also predicts that the core formation time is about three times shorter than that with no turbulence, when the turbulent speed is comparable to the Alfvén speed.

22 pages, 9 figures, accepted for publication in ApJ

References in corpus (6)

• Theory of Star Formation
• On the Rapid Collapse and Evolution of Molecular Clouds
• Magnetically Aligned Velocity Anisotropy in the Taurus Molecular Cloud
• Optical polarimetry toward the Pipe nebula: Revealing the importance of the magnetic field
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Cited by in corpus (8)

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• Magnetic Field Structure of Dense Cores using Spectroscopic Methods
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• Distortion of Magnetic Fields in a Starless Core VI: Application of Flux Freezing Model and Core Formation of FeSt 1-457
• Fitting an Analytic Magnetic Field to a Prestellar Core
• Magnetic field measurement in TMC-1C using 22.3 GHz CCS Zeeman splitting
• The Magnetic Field versus Density relation in Star-Forming Molecular Clouds