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Dynamics of the superfine structure in the Orion KL jet

Published online by Cambridge University Press:  03 August 2017

Leonid I. Matveyenko ,
Phil J. Diamond  and
David A. Graham
Leonid I. Matveyenko
Affiliation:
Space Research Institute, Profsojuznaja 84/32, 117810 Moscow, Russia
Phil J. Diamond
Affiliation:
Nuffield Radio Observatory, Macclesfield, Cheshire SK11, 9DL, UK
David A. Graham
Affiliation:
Max-Planck-Institut für Radioastronomie, Auf dem Hügel 69, 53121, Bonn, Germany

Abstract

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We have studied the superfine structure of the active H2O maser region in Orion KL with an angular resolution of ≤ 0.3 × 0.7 mas. The high level of H2O maser emission from 1979-1988 was due to an accretion disk, which is divided into five groups of protoplanetary rings. The peak brightness temperatures of the structures was Tpeak = 1013-14 K. The region is located in the OMC-1 molecular cloud, VLSR ⋍ 7.74 km/s. The cloud amplifies by more than two orders of magnitude the emission from the structures, whose radial velocities are within the maser window ±0.3 km/s. Due to this, the velocity of the H2O super maser emission is constant. In the quiescent period of 1995 a 6 AU jet was discovered, PA = −32°, Tb ⋍ 1011K. In 1998 the jet's brightness temperature increased by more than 3 orders of magnitude. Initially the jet's position angle was PA = −45°, and then changed to PA = −38°. During the period of decreasing emission in 1999 the jet had changed its form and became a helix, that suggests the precession of the rotation axes. In the central part of the jet there is a compact bright source - “the ejector” - with Tejc = 1017 K.

Type
Part 1. Star Formation
Information
Symposium - International Astronomical Union , Volume 206: Cosmic Masers: From Protostars to Blackholes , 2002 , pp. 96 - 99
Copyright
Copyright © Astronomical Society of the Pacific 2002 

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