2003ApJ...588..478G

We have monitored the SiO (v=1, J=2⟶1) maser polarization in 17 variable stars (Miras, OH-IR stars, and supergiants) to investigate the long-term persistence of masers. The eight epochs of observations span 2.5 yr, thereby sampling multiple cycles for these stars with typical periods of ∼1 yr. The average polarization was 23% with a typical dispersion of 7%, although the variability differed substantially from star to star. In the Stokes q and u spectra of individual stars, a few strong maser features tended to dominate the polarization, with the maser features persisting for less than one stellar cycle for some stars, and for multiple cycles for a few stars. Because individual masers are not resolved in our beam-averaged total intensity spectra, we correlated the polarization spectra between epochs to measure the characteristic lifetimes of the features, rather than attempting to trace the evolution of separate line components. We found that individual maser feature lifetimes ranged from a few months or less to more than 2 yr. These data indicate that for the sample of stars as a whole, the masers are not reset at a particular stellar phase.