Further VLBA observations of SiO masers toward Mira variable stars

Details Further VLBA observations of SiO masers toward Mira variable stars Further VLBA observations of SiO masers toward Mira variable stars

Sep 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006a%26a...456..339c&link_type=abstract

Astronomy and Astrophysics, Volume 456, Issue 1, September II 2006, pp.339-350

Astronomy and Astrophysics

Astrophysics

25

Stars: Atmospheres, Stars: Agb And Post-Agb, Stars: Variables: General, Radio Lines: Stars, Masers

Scientific paper

We present the results of continued monitoring of the SiO masers at 7 mm wavelength in several of the Mira variable stars reported in Cotton et al. (2004, A&A, 414, 275) (o Ceti = Mira, U Orionis = U Ori, R Aquarii = R Aqr) over a period of 16 months, extending the observations to several pulsation cycles. The observed size of the maser rings varied by 3-14% with time but show no clear correlation with pulsation phase. In all cases, the SiO masers appear just outside the dense molecular layer indicated by near-IR observations. Rotation (or large scale motion) is possibly detected in o Ceti with a period of 89× sin(i) years. We find linear polarization up to ˜ 60% and at several epochs predominantly tangentially ordered polarization vectors indicate a radial magnetic field direction. Jet-like features are examined in o Ceti and R Aqr and in both cases, the magnetic field appears elongated with the masing structure. This suggests that the dynamic feature in the envelope is dragging the magnetic field or that the gas is constrained to follow magnetic field.

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