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H2O megamaser in Orion KL

Published online by Cambridge University Press:  23 September 2016

L.I. Matveyenko
L.I. Matveyenko*
Affiliation:
Space Research Institute Profsojuznaja 84 Moscow V 485 U.S.S.R.

Abstract

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The region of the H2O megamaaer emission in Orion KL had been studied by VLBI method. The structure is a chain of the compact components oriented under the angle X ≅ −80°. The size of the components is ⩽ 0.1 A.U., the brightness temperature Tb ≅ 1017 K, the linewidth of each component is Δ f ⋜ 7 kHz. The emission has linear polarization P ⋝ 80 % and position angle is changed by 9.2 degree / A.U. The velocity of the components has a gradient 0.41 km/sec A.U. The masers are unsaturated, the kinetic temperature Tk ≤ 120 K. The structure corresponds to an expanding protoplanet rings, radius of which is equal R = 6 A.U. The rotation and the expanding velocities are equal 5 and 3.8 km/s accordingly. Mass of a protostar is ~ 0.7 M⊙.

Type
III Flare Stars and Related Objects Fuors and Other Non-Stable Objects
Information
Symposium - International Astronomical Union , Volume 137: Flare Stars in Star Clusters, Association and Solar Vicinity , 1990 , pp. 271 - 274
Copyright
Copyright © Kluwer 1990 

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