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Unveiling the Role of the Magnetic Field at the Smallest Scales of Star Formation

  • Authors: Charles L. H. Hull, Philip Mocz, Blakesley Burkhart, Alyssa A. Goodman, Josep M. Girart, Paulo C. Cortés, Lars Hernquist, Volker Springel, Zhi-Yun Li, and Shih-Ping Lai

2017 The Astrophysical Journal Letters 842 L9.

  • Provider: AAS Journals

Caption: Figure 2.

Multi-scale projections of simulated data. Shown are the column densities and the magnetic field orientation of protostellar cores that formed in our AREPO simulations. As indicated, the initial mean magnetic field is oriented in the vertical direction. The initial magnetic field strength increases from the left to the right columns, corresponding to Alfvén Mach numbers ﹩{{ \mathcal M }}_{{\rm{A}},\mathrm{mean} \mbox{-} \mathrm{field}}=35,3.5,1.2,0.35﹩ (see Table 1). The top row shows the full-scale AREPO simulations, centered on the cores shown in the bottom row. The full simulation boxes are 5.2 pc in extent (cloud scale). The middle row shows zoom-ins between JCMT and CARMA scales (core scale). The bottom row shows zoom-ins of cores at ALMA scales (protostar scale). By allowing the magnetic field orientations and zoom boxes to be toggled on and off, the interactive figure enables the reader to compare more easily the background grayscale column density maps with the foreground magnetic field orientations.

(An interactive version of this figure is available.)

An interactive version of this figure is available in the online journal.

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