Astron. Astrophys. Suppl. Ser. 141, 185-192
Send offprint request: E.E. Lekht
1 - Instituto Nacional de Astrofísica, Óptica y Electrónica, Luis Enrique Erro No. 1, Apdo Postal 51 y 216, 72840 Tonantzintla, Puebla, Mexico
2 - Sternberg Astronomical Institute, 13 Universitetskij prospekt, Moscow 119899, Russia
Received December 8, 1998; accepted August 6, 1999
The evolution of emission of the 42.2 km s-1 maser condensation is traced at a timespan of 16 years. The flux density was plotted versus linewidth for this feature (in the coordinates). This dependence contains two branches, largely shifted with respect to each other. The transition from one branch to the other took 2.5 years, while the linewidth was fluctuating. Possible causes of existence of the two branches in the maser emission evolution are discussed.
An analysis of the entire data set for 1976-1998 has shown that the time interval between the minima of integral flux in G43.8-0.1 was 18 1 yr. This figure can be taken as the period of the H2O maser activity in G43.8-0.1.
Key words: masers -- stars: formation -- radio lines: stars
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