Variations of the H2O Maser Emission of W51M in 1981-1998

Details Variations of the H2O Maser Emission of W51M in 1981-1998 Variations of the H2O Maser Emission of W51M in 1981-1998

May 2001

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001arep...45..339s&link_type=abstract

Astronomy Reports, Volume 45, Issue 5, May 2001, pp.339-349

Astronomy and Astrophysics

Astronomy

1

Scientific paper

The results of spectral monitoring of the maser source W51M carried out in the water-vapor line at 1.35 cm (22GHz) on the 22-m telescope of the Pushchino Radio Astronomy Observatory in 1981 1998 are reported and interpreted. Long-term variations of the maser flux with a period of 12 13 years are found. W51M may be a rotating and simultaneously expanding toroidal cloud of gas and dust around a young star with a mass of the order of ˜15M &sun;, with numerous high-velocity jets of maser condensations flowing out in two broad cones along the polar axis of the torus. A stellar wind with a velocity of about 2000 3000 km/s is responsible for the maser pumping.

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