Abstract SiO maser VLBA observations toward VX Sgr are performed at five epochs, and lots of maser spots are obtained. We make a statistical analysis on these spots. It is shown that the apparent sizes and the fluxes of maser spots decrease with increasing the distance from the central star. In addition, the similarity between the v = 1,2 (J=1–0) spectrums increases with epochs, consistent with the full width at half maximum (FWHM), while the total fluxes increase. The results may be related to the changeable pumping mechanisms.
Keywords masers — stars: individual (VX Sgr) — techniques: interferometric — turbulence
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