Computer Science
Scientific paper
Jan 2001
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001iaus..205..258m&link_type=abstract
Galaxies and their Constituents at the Highest Angular Resolutions, Proceedings of IAU Symposium #205, held 15-18 August 2000 at
Computer Science
Scientific paper
The structures, consisting of a protostar, an accresion disk, and a bipolar jet, are discovered in two active zones of the gas-dust complex of the Orion Nebula. The star-forming regions are spaced at distance of 1500 AU and located within the molecular cloud OMC-1. The disks are separated into protoplanetary rings. The H2O maser emission of the rings is concentrated in the azimuthal plane. The radial velocity of the cloud is VLSR = -7.74 km/s. The brightness temperatures of the components whose radial velocities are within the OMC-1 maser window, increase by two orders. The optical depth of the maser is τ ≈5 for the unsaturated regime. In the first period of the high activity (1971-1987) epoch the supermaser emission was determined by the rings, the planes of which was oriented parallel to the line of sight. After activity decreased (quiescent period) the maser emission is related with the bipolar structure. That bipolar outflow - jet determines the H2O supermaser emission over the second period of high activity. The emission of the jet has a strong linear polarization. A similar structure is observed in the second region.
Diamond Phil J.
Graham David A.
Matveyenko L. I.
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