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Variations of the H2O maser emission of W51M in 1981–1998

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Abstract

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 ⊙, 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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Authors and Affiliations

  1. Pushchino Radio Astronomy Observatory, Astro Space Center, Lebedev Institute of Physics, Pushchino, Moscow oblast, 142292, Russia

    V. A. Samodurov & S. V. Logvinenko

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  1. V. A. Samodurov
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  2. S. V. Logvinenko
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__________

Translated from Astronomicheski\(\overset{\lower0.5em\hbox{$\smash{\scriptscriptstyle\smile}$}}{l}\) Zhurnal, Vol. 78, No. 5, 2001, pp. 396–407.

Original Russian Text Copyright © 2001 by Samodurov, Logvinenko.

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Samodurov, V.A., Logvinenko, S.V. Variations of the H2O maser emission of W51M in 1981–1998. Astron. Rep. 45, 339–349 (2001). https://doi.org/10.1134/1.1369797

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