OMC-1: A Cool Arching Filament in a Hot Gaseous Cavity: Geometry, Kinematics, Magnetic Vectors, and Pressure Balance

Details OMC-1: A Cool Arching Filament in a Hot Gaseous Cavity: Geometry, Kinematics, Magnetic Vectors, and Pressure Balance OMC-1: A Cool Arching Filament in a Hot Gaseous Cavity: Geometry, Kinematics, Magnetic Vectors, and Pressure Balance

Mar 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007aj....133.1012v&link_type=abstract

The Astronomical Journal, Volume 133, Issue 3, pp. 1012-1026.

Astronomy and Astrophysics

Astronomy

7

Dust, Extinction, Infrared: Ism, Ism: Magnetic Fields, Polarization, Stars: Formation

Scientific paper

We have assembled data on large (Galactic shell), middle (filament), and small (protostar) scales. OMC-1 is embedded in a hot cavity. Here we have made multiconstituent (gas/dust/field) homogeneous maps of the central part of the OMC-1 filament, covering an area of 2'×2'. We find here that the vertical filament has a turbulent pressure about equal to the magnetic pressure; its total pressure roughly equals that in the surrounding medium. The magnetic field crosses the filament with an estimated strength of 300-350 μG in the sky plane. It could be an ``externally wrapped'' U-shaped magnetic field going around the filament (due to a large shock front traveling in the cavity), or else an internally generated ``helical'' field (of unknown origin). Near the OMC-1 map center, we map the low-velocity outflow near IRc2-source I, with a pattern of blue south-southwest gas and red north-northeast gas. Our James Clerk Maxwell Telescope data yield a plane-of-sky field of 2.4-2.6 mG across the outflow; this strength nearly equals the published Zeeman line-of-sight data. Farther out, the Zeeman data show a negative magnetic field, possibly suggesting a pole-on dipolar field.

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