Subarcsec Polarization Images of 86 GHz SiO Emission in Orion-IRc2

Details Subarcsec Polarization Images of 86 GHz SiO Emission in Orion-IRc2 Subarcsec Polarization Images of 86 GHz SiO Emission in Orion-IRc2

May 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002aas...200.8501p&link_type=abstract

American Astronomical Society, 200th AAS Meeting, #85.01; Bulletin of the American Astronomical Society, Vol. 34, p.785

Astronomy and Astrophysics

Astronomy

Scientific paper

To probe the magnetic field morphology near the massive young star Orion-IRc2, we used the BIMA array to map the linear polarization of the J=2-1 SiO masers, in both the v=1 and v=0 vibrational levels, with 0.4'' angular resolution. The strong v=1 masers are confined to a narrow zone 40 AU from the star. These masers have fractional polarizations of a few percent. The polarization position angle tends to correlate with the maser intensity, and fluctuates on time scales of years. For the v=1 masers the stimulated emission rate R is much greater than the Zeeman splitting gΩ due to any plausible magnetic field, so the maser polarization need not be correlated with the field direction. The much weaker v=0 masers originate 500 AU from IRc2, in what appears to be a flared disk. For these masers we measure a position angle PA ~80°, constant in time and varying little across the line profile. By contrast, Tsuboi et al. (1996) measured PA ~150°\ for the J=1-0 v=0 SiO transition. Possibly this discrepancy is attributable to Faraday rotation by plasma in the foreground H 2 region. If so, the intrinsic polarization angle is ~55°, parallel to the plane of the circumstellar disk. If the disk is seen edge-on, then the magnetic field threads the disk poloidally, with relatively little pinch. This work was supported by NSF grant AST-21795.

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