Abstract
Abstract We present two-epoch maps of SiO masers ($v=$ 1 and $v=$ 2, $J=$ 1-0) associated with the M-type star IRC$-$10414, which were obtained with the Japanese VLBI Network (JVN). The spatial and Doppler velocity distributions, and the intensity ratio of the $v=$ 1 to $v=$ 2 ($J=$ 1-0) lines have significantly changed for eight years since our previous Very Long Baseline Array (VLBA) observation. The maser proper motions revealed by these two-epoch observations with an interval of one month are quite random and too fast to be explained by ballistic motions of the maser clumps. The maser distributions seen in the present observations cannot be explained by a rotating-infalling ring model implied in the previous work. We discuss the kinematical relation between the SiO and H$_{2}$O masers in IRC$-$10414. In the present observations, the scale sizes of SiO $v=$ 1 and $v=$ 2 masers in IRC$-$10414 were roughly equal, as observed in typical Mira variables.
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