Computer Science
Scientific paper
Sep 1984
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984esasp.213..179m&link_type=abstract
In ESA QUASAT: A VLBI Obs. in Space p 179-180 (SEE N85-16700 07-88)
Computer Science
Interstellar Masers, Orion Nebula, Water Masers, Brightness Temperature, Interstellar Radiation, Quasat, Spectral Emission, Stellar Evolution
Scientific paper
A powerful H2O maser outburst was observed in the Orion Nebula in August-September 1979. Flux density reached 2 million Jy; component velocity = 8 km/sec. The line profile is asymmetric and time variable. The outburst region has components located along the direction minus 50 deg. Line width depends on the emission region size-differential velocity and, under the assumption of a point source, corresponds to a 7 kHz line width. This is evidence of the low temperature of a maser cloud, 60 K. The line emission is mainly from its central region the size of which is 1 mas, i.e., 0.5 AU and the brightness temperature = 10 to the 16th power K. The intricate fine structure of the profile suggests the presence of compact components within the region, which are 0.1 AU and whose brightness temperature is 10 to the 17th power K. A high angular resolution, e.g., QUASAT VLBI satellite, study is required to understand the outbursts.
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