The H2O maser flare in Orion A

Details The H2O maser flare in Orion A The H2O maser flare in Orion A

Dec 1982

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1982pazh....8..711m&link_type=abstract

(Pis'ma v Astronomicheskii Zhurnal, vol. 8, Dec. 1982, p. 711-713) Soviet Astronomy Letters (ISSN 0360-0327), vol. 8, Nov.-Dec.

Astronomy and Astrophysics

Astronomy

5

Hydrogen Clouds, Interstellar Masers, Water Masers, Brightness Temperature, Interferometry, Line Spectra, Radio Emission

Scientific paper

The values of the visibility function are found to vary within the line profile, with gamma being larger at the lower frequencies. This effect is more marked for the longer baseline, suggesting that the high-frequency emission region has a larger angular size than the low-frequency region and that one of the regions is partially resolved even by the shorter baseline. The data imply that a compact 0.0005-arcsec (0.25 AU) core is embedded in an extended halo that is approximateley 0.006 arcsec (3 AU) across. The flare emission is seen as emanating from a compact core of 0.0005 arcsec, responsible for 65 percent of the radio flux, and a halo about 0.005 arcsec in diameter, which accounts for the remaining 35 percent. The brightness temperatures of the two components are 5 x 10 to the 16th K and 3 x 10 to the 14th K, respectively. The high brightness temperature found for the flare regions indicates that the emission may be sharply directional, whether because of the masing mechanism itself (coherence) or the source geometry (strongly elongated). It is pointed out that the source could present such a configuration if it were a protoplanetary ring whose plane is oriented edgewise to the observer.

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