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A&A Supplement Series, Vol. 126, December I 1997, 257-266

Received June 5, 1996; accepted March 5, 1997

Evolution of tex2html_wrap_inline1152 maser emission in the direction of the semiregular variable RT Virginis during 1985-1996

J.E. Mendoza-Torres tex2html_wrap1174 - E.E. Lekht tex2html_wrap1174 - I.I. Berulis tex2html_wrap1178 - M.I. Pashchenko tex2html_wrap1180

Send offprint request: J.E. Mendoza-Torres
tex2html_wrap1182 Instituto Nacional de Astrofísica, Optica y Electrónica, Apartado Postal 51 y 216, Puebla, Pue., Z.P. 72000, México
tex2html_wrap1182  Astro-cosmic centre of Lebedev Physical Institute, Russian Academy of Siences, Leninskij prospect 53, 117912, Moscow, Russia
tex2html_wrap1184  Technological University, Kaunas, Lithuania
tex2html_wrap1186  Sternberg Astronomical Institute, Universitetsky prospect 13, 119899, Moscow, Russia


We present a catalog of the 22 GHz tex2html_wrap_inline1154 maser profiles of the semiregular variable RT Vir. The observations were made from 1985 to 1996 at the RT-22 radio telescope of the Radio Astronomical Station at Pushchino, Russia. Results obtained after the analysis of the integrated fluxes, the average spectra, the centroid velocity and the superposition of the spectra are reported.

Anticorrelation of the integrated fluxes of two spectral intervals (tex2html_wrap_inline1158 and tex2html_wrap_inline1160) was found. The characteristic time variation of the maser emission at each of these groups was about 5-6 years. This phenomenon may be explained by a variation of the outflow of the matter from the star. The outflow is weakly bipolar. We can suppose that in such a model the enhancement of the outflow occured alternately with a period of about 5-6 years. The anticorrelation of the integrated fluxes of two groups of maser features, located symmetrically relative to the star, may be a result of this alternation.

keywords: RT Vir -- radio lines: masers -- stars: variables: other

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