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Paper: Fine Structure of Star Formation Region in Orion KL
Volume: 402, Approaching Micro-Arcsecond Resolution with VSOP-2: Astrophysics and Technologies
Page: 372
Authors: Matveyenko, L.; Diamond, P.J.; Graham, D.A.; Zaharin, K.M.; Demichev, V.A.; Sivakon, S.S.
Abstract: A star formation region in Orion KL is studied in H2O maser emission. The structure consists of an accretion disk, a bipolar outflow, and an envelope. The disk is divided into rings with a rotation velocity vrot ≃ΩR, period T ≃ 170 yr. The kinetic energy of rotation transforms into the bipolar outflow v ∼ 10 km/s. The reactive force leads to two-mode precession and forms the outflow of a helix structure with a curved axis. The disk is the accreted environment in the azimuth plane and is ejected along the rotation axis like vortexes. A shell amplifies emission more than two orders at V=7.65 km/s. The ejector size is ≤ 50μas, and the brightness temperature Tb ≥ 1017K.
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