Volume 376, Number 3, September IV 2001
|Page(s)||928 - 940|
|Section||Interstellar and circumstellar matter|
|Published online||15 September 2001|
Variability of the H2O maser associated with the Mira variable RS Virginis
Instituto Nacional de Astrofísica, Óptica y Electrónica, Luis Enrique Erro No. 1, Apdo Postal 51 y 216, 72840 Tonantzintla, Puebla, México
2 Sternberg Astronomical Institute, 13 Universitetskij prospekt, Moscow 119899, Russia e-mail: firstname.lastname@example.org
3 Pushchino Radio Astronomy Observatory, Astrospace Center of the Lebedev Institute of Physics, Russian Academy of Sciences, Pushchino, Moscow Region 142290, Russia e-mail: email@example.com
Corresponding author: E. E. Lekht, firstname.lastname@example.org; email@example.com
Accepted: 2 July 2001
The results of observations of the H2O maser emission ( cm) of the Mira-type variable star RS Vir are presented. The observations were carried out in 1981-2001 () on the RT-22 radio telescope of the Pushchino Radio Astronomy Observatory (Russia). The variability curve of the H2O maser emission integrated flux Fint(H2O) of RS Vir correlates with its visual light curve with some phase delay (P is the star's period). The delay variations seem to be periodic at a timescale of 19-20 years ("superperiod" of the maser variations). If the variability of the H2O maser RS Vir is caused by periodic action of pulsation-driven shock waves, the shock travel time from the photosphere to the inner boundary of the H2O maser shell can be as long as (3-5)P. Another explanation is that maser variations may be connected with changing gas density in the masering region of the circumstellar envelope. In particular, long-term maser variations (the "superperiod" ) may be caused by changing mass loss rate .
Key words: stars: variables: general / circumstellar matter / stars: individual: RS Vir / radio lines: stars / masers / shock waves
© ESO, 2001
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