Variability of the H2O maser associated with the M-supergiant S Persei

Details Variability of the H2O maser associated with the M-supergiant S Persei Variability of the H2O maser associated with the M-supergiant S Persei

Jul 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005a%26a...437..127l&link_type=abstract

Astronomy and Astrophysics, Volume 437, Issue 1, July I 2005, pp.127-133

Astronomy and Astrophysics

Astrophysics

6

Stars: Agb And Post-Agb, Circumstellar Matter, Stars: Mass-Loss, Stars: Supergiants, Masers, Stars: Late-Type

Scientific paper

We present the results from observing the circumstellar maser emission of the M-type supergiant S Per in the 6{16}-5{23} water-vapour line at 1.35 cm. The observations were carried out in 1981-2002 (JD=2 444 900-2 452 480) 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 P≈ 800 d is the mean light cycle for S Per. The feature at VLSR=-44 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.

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