Polarization properties and time variations of the SiO maser emission of W Hydrae

Details Polarization properties and time variations of the SiO maser emission of W Hydrae Polarization properties and time variations of the SiO maser emission of W Hydrae

Feb 1985

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985apj...289..756c&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 289, Feb. 15, 1985, p. 756-764. Research supported by the University of Ken

Astronomy and Astrophysics

Astrophysics

17

Emission Spectra, Interstellar Masers, Linear Polarization, Silicon Oxides, Stellar Envelopes, Variable Stars, Line Spectra, Polarization Characteristics

Scientific paper

The polarization properties of the v = 1, J = 2-1 SiO circumstellar maser emission from W Hya have been measured over a period of 3.5 yr. Data are presented concerning Stokes parameter I and linear polarization. The W Hya line profiles exhibit peaks which are well represented by a superposition of a small number of narrow Gaussian features, each having a well-defined position angle of maximum linear polarization. These features seen to persist for an optical period and then disappear near optical maximum. The disappearance of the features may be due to the passage of periodic atmospheric shock waves. The data offer the first evidence for a small velocity pulsation in the SiO maser emission features which may be related to the envelope pulsation observed in the infrared. From the data it is argued, as for R Leo, that the SiO maser is located extremely close to the star, and that the dominant gain path is likely to be tangent to the stellar surface. Based on certain peculiarities in the data, it is suggested that the shell of circumstellar material sampled by the SiO maser may be somewhat thicker for W Hya than for stars previously observed in the program.

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