Journal
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
Volume 470, Issue 3, Pages 2938-2948Publisher
OXFORD UNIV PRESS
DOI: 10.1093/mnras/stx1381
Keywords
MHD; stars: formation; ISM: clouds; ISM: kinematics and dynamics; ISM: structure
Categories
Funding
- US Department of Energy [GR523126]
- National Science Foundation [GR506177]
- Space Telescope Science Institute [GR528562]
- Canadian Institute for Theoretical Astrophysics (CITA) National Fellowship
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We present numerical simulations of reorienting oblique shocks that form in the collision layer between magnetized colliding flows. Reorientation aligns post-shock filaments normal to the background magnetic field. We find that reorientation begins with pressure gradients between the collision region and the ambient medium. This drives a lateral expansion of post-shock gas, which reorients the growing filament from the outside-in (i.e. from the flow/ambient boundary, towards the colliding flows axis). The final structures of our simulations resemble polarization observations of filaments in Taurus and Serpens South, as well as the integral-shaped filament in Orion A. Given the ubiquity of colliding flows in the interstellar medium, shock reorientation may be relevant to the formation of filaments normal to magnetic fields.
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