Abstract
The superfine structure of the active region in Orion KL has been investigated in the H2O maser line at two epochs, December 23, 1998, and April 24, 1999, with an angular resolution as high as 0.01 mas. A bright central source, a bipolar outflow ejector with two nozzles spaced 0.008 mas apart, has been identified. The impact of the ejected flows causes precession of the rotation axis and gives rise to a jet structure in the shape of diverging helixes of opposite signs. The longitudinal velocities of the flows differ by 0.12 km s−1. The flow emission at the exit from the nozzles is linearly polarized and oriented at an angle of 22° relative to the rotation axis or parallel to the flow velocities. Their brightness temperature exceeds T b > 1018 K. The width of the emission line profiles is 0.43 km s−1, their relative shift is ±0.06 km s−1, and the orientations of the polarization planes differ by 45°, which determines the extraordinary rotation of the polarization plane, 25°/km s−1.
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Original Russian Text © L.I. Matveyenko, S.S. Sivakon’, 2008, published in Pis’ma v Astronomicheskiĭ Zhurnal, 2008, Vol. 34, No. 12, pp. 908–919.
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Matveyenko, L.I., Sivakon’, S.S. Polarized emission from the ejector in Orion KL. Astron. Lett. 34, 820–831 (2008). https://doi.org/10.1134/S1063773708120025
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DOI: https://doi.org/10.1134/S1063773708120025