Volume 437, Number 1, July I 2005
|Page(s)||127 - 133|
|Section||Interstellar and circumstellar matter|
|Published online||10 June 2005|
Variability of the H2O maser associated with the M-supergiant S Persei
Instituto Nacional de Astrofísica, Óptica y Electrónica, Luis Enrique Erro No. 1, Apdo Postal 51 y 216, 72840 Tonantzintla, Puebla, México e-mail: [lekht;mend]@inaoep.mx
2 Sternberg Astronomical Institute, 13 Universitetskij prospekt, Moscow, 119992 Russia e-mail: email@example.com
3 Pushchino Radio Astronomy Observatory, Astrospace Center of the Lebedev Institute of Physics, Russian Academy of Sciences, Pushchino, Moscow Region, 142290 Russia e-mail: firstname.lastname@example.org
Accepted: 3 February 2005
We present the results from observing the circumstellar maser emission of the M-type supergiant S Per in the 616–523 water-vapour line at 1.35 cm. The observations were carried out in 1981–2002 (–2 452 480) on the RT-22 radio telescope of the Pushchino Radio Astronomy Observatory, Astrospace Center of the Lebedev Institute of Physics, Russian Academy of Sciences. The H2O spectra obtained represent an unprecedented long, uniform dataset on this star. We discuss the properties of the optical and maser variations of S Per, together with particulars of the available VLBI maps. The close relation between maser and optical variations favors a model in which mass-loss is episodic. Changes observed in the total H2O line flux follow the visual light curve with a delay of 0.01 to 0.5P, where d is the mean light cycle for S Per. The feature at km s-1 flared in July 1988, which seemed to be the response of the maser to an unusually bright optical maximum. The position of the -44-km s-1 feature on the VLBI maps coincides with the direction toward the optical stellar disc, which can be explained by amplification of enhanced stellar continuum by the H2O line.
Key words: stars: AGB and post-AGB / circumstellar matter / stars: mass-loss / stars: supergiants / masers / stars: late-type
© ESO, 2005
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