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Twenty-six-year monitoring of water masers

Published online by Cambridge University Press:  01 March 2007

G. M. Rudnitskij ,
M. I. Pashchenko ,
V. F. Esipov ,
V. A. Samodurov ,
I. A. Subaev ,
A. M. Tolmachev  and
E. E. Lekht
G. M. Rudnitskij
Affiliation:
Sternberg Astronomical Institute, Moscow State University, 13 Universitetskij prospekt, Moscow, 119992 Russia email: [email protected]
M. I. Pashchenko
Affiliation:
Sternberg Astronomical Institute, Moscow State University, 13 Universitetskij prospekt, Moscow, 119992 Russia email: [email protected]
V. F. Esipov
Affiliation:
Sternberg Astronomical Institute, Moscow State University, 13 Universitetskij prospekt, Moscow, 119992 Russia email: [email protected]
V. A. Samodurov
Affiliation:
Pushchino Radio Astronomy Observatory, Astrospace Center of the Lebedev Institute of Physics, Russian Academy of Sciences, Pushchino, Moscow Region, 142290 Russia email: [email protected]
I. A. Subaev
Affiliation:
Pushchino Radio Astronomy Observatory, Astrospace Center of the Lebedev Institute of Physics, Russian Academy of Sciences, Pushchino, Moscow Region, 142290 Russia email: [email protected]
A. M. Tolmachev
Affiliation:
Pushchino Radio Astronomy Observatory, Astrospace Center of the Lebedev Institute of Physics, Russian Academy of Sciences, Pushchino, Moscow Region, 142290 Russia email: [email protected]
E. E. Lekht
Affiliation:
Sternberg Astronomical Institute, Moscow State University, 13 Universitetskij prospekt, Moscow, 119992 Russia email: [email protected] Instituto Nacional de Astrofísica, Óptica y Electrónica, Luis Enrique Erro No. 1, Apdo Postal 51 y 216, 72840 Tonantzintla, Puebla, México email: [email protected]
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Abstract

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Since 1980 variability of a sample of H2O maser sources has been monitored on the 22-metre radio telescope in Pushchino, Russia. The interval between successive observational sessions is 1–2 months. The sample includes 125 maser sources in star-forming regions (SFR) and late-type variable stars. Twenty-six-year time series of H2O line profiles have detected flares and velocity drift of spectral features. Very fast variations in the H2O maser flux (Δt ≲ 1 hour) have been detected in several SFR sources, in particular, W33B. Variations of circumstellar H2O masers in late-type stars correlate with visual light curves with a time lag of 0.3-0.4P (P is the star's period). Exceptionally strong H2O maser flares were recorded in SFR sources (Sgr B2 and others) and in the stars W Hya, R Cas and U Ori. Models for H2O maser variability are reviewed. For stellar masers shock-wave excitation of H2O line variability is discussed.

Keywords

molecular processesradio lines: ISMradio lines: starsmaserssurveysstars: formationstars: AGB and post-AGBcircumstellar mattershock waves
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 3 , Symposium S242: Astrophysical Masers and their Environments , March 2007 , pp. 330 - 331
Copyright
Copyright © International Astronomical Union 2008

References

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