Flares of the H2O Maser in W31(2)

Details Flares of the H2O Maser in W31(2) Flares of the H2O Maser in W31(2)

May 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005astl...31..315l&link_type=abstract

Astronomy Letters, vol. 31, Issue 5, p.315-326

Astronomy and Astrophysics

Astronomy

3

Star Formation - Water-Vapor Maser Emission

Scientific paper

We analyze our monitoring data for the water-vapor maser in the source W31(2), associated with a region of vigorous star formation, a cluster of OB stars. The monitoring was performed with the 22-m radio telescope at Pushchino Radio Astronomy Observatory during 1981 2004. The variability of the H2O maser in W31(2) was found to be cyclic, with a mean period of 1.9 yr. Two flares were most intense (superflares): in 1985 1986 and 1998 1999. In each activity cycle, we observed up to several short flares, subpeaks. The fluxes of many emission features during the flares were correlated. We also observed successive activation of individual emission features in order of increasing or decreasing radial velocity, suggesting an ordered structure and, hence, a radial-velocity gradient of the medium. There is a clear correlation of the emission peaks of the main components in the spectra at radial velocities of -1.7, -1.3, 0.5, and 1.3 km s-1 with activity cycles and of the emission at VLSR < -8 km s-1 with short flares. During the superflares, the emission in the low-velocity part of the H2O spectrum and a number of other phenomena related to coherent maser-emission properties were suppressed. The maser spots are assumed to form a compact structure, to have a common pumping source, and to be associated with an accretion flow onto the cluster of OB stars.

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