Long-Term Monitoring of the Long-Period Variable Y Cassiopeiae in the 1.35-cm Water-Vapor Line

Details Long-Term Monitoring of the Long-Period Variable Y Cassiopeiae in the 1.35-cm Water-Vapor Line Long-Term Monitoring of the Long-Period Variable Y Cassiopeiae in the 1.35-cm Water-Vapor Line

Nov 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005astl...31..760r&link_type=abstract

Astronomy Letters, vol. 31, Issue 11, p.760-766

Astronomy and Astrophysics

Astronomy

1

Late-Type Stars - Long-Period Variable Stars - Circumstellar Envelopes - Maser Radio Sources

Scientific paper

Observations of the circumstellar maser emission from the long-period variable star Y Cas in the 1.35-cm water-vapor line are presented. The observations were performed with the RT-22 radio telescope at the Pushchino Radio Astronomy Observatory (Astrospace Center, Lebedev Physical Institute, Russian Academy of Sciences) in the period 1982 2005. The variations in the integrated flux F int in the H2O line correlate with the visual light curve of the star. The phase delay Δϕ between the F int variations and the light curve is 0.2 0.4P (P is the period of the star). The H2O maser Y Cas belongs to transient sources: peaks of high maser activity alternate with intervals of a low emission level when the H2O-line flux does not exceed (0.1 0.5) × 10-20 W m-2. A “superperiod” of ˜5.7 yr was found in the occurrence of activity peaks. A particularly strong maximum of maser radio emission took place at the end of 1997, when the flux F int reached 15.6 × 10-20 W m-2. A model for the H2O maser variability in Y Cas is discussed. The variability is caused by a periodic action of shock waves driven by stellar pulsations. The H2O maser flares may be associated with short-lived episodes of enhanced mass loss by the star or with the propagation of a particularly strong shock wave when a planet orbiting the star passes through its periastron.

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