Star formation region in Orion KL. epoch 1985.8

We have derived the fine structure of the region of the H2O supermaserflare in the Orion Nebula at epoch 1985.8. This structure includes a chain of compact components that extends to 25 AU and has a width of 0.4 AU. The velocities of the components vary along the chain. The structure corresponds to...

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Bibliographic Details
Published in:Astronomy reports 2004-12, Vol.48 (12), p.979-987
Main Authors: Demichev, V A, Matveenko, L I
Format: Article
Language:English
Subjects:
Accretion
Accretion disks
Star & galaxy formation
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Summary:We have derived the fine structure of the region of the H2O supermaserflare in the Orion Nebula at epoch 1985.8. This structure includes a chain of compact components that extends to 25 AU and has a width of 0.4 AU. The velocities of the components vary along the chain. The structure corresponds to an accretion disk separated into protoplanetary rings, viewed edge-on. The velocities of the components correspond to Keplerian motion around an object with a mass of M=0.3-0.2M {circled dot}. The velocity of the central object relative to the Local Standard of Rest is V LSR=4.0-0.7 km/s. The radius of the inner part of the disk is 9-4 AU, while the radius of the outer disk is 35-6 AU. The rotational velocities of the inner and outer rings are 5-1 km/s and 2.5-0.5 km/s, respectively. The emission of the structure is amplified in the ambient medium--an envelope with velocities of 7.6-0.3 km/s. The rate at which the envelope is accreting onto the central object is 3.6-0.7 km/s. The gradient of the infall velocity is 1.1 km/s.
ISSN:1063-7729
1562-6881
DOI:10.1134/1.1836021