  A single dish monitoring of millimeter maser lines SiS J=14-13 and HCN nu_2 =
1^f J=3-2 and several other rotational lines is reported for the archetypal
carbon star IRC+10216. Relative line strength variations of 5%~30% are found
for eight molecular line features with respect to selected reference lines.
Definite line-shape variation is found in limited velocity intervals of the SiS
and HCN line profiles. The asymmetrical line profiles of the two lines are
mainly due to the varying components. Their dominant varying components of the
line profiles have similar periods and phases as the IR light variation,
although both quantities show some degree of velocity dependence; there is also
variability asymmetry between the blue and red line wings of both lines.
Combining the velocities and amplitudes with a wind velocity model, we suggest
that the line profile variations are due to SiS and HCN masing lines emanating
from the wind acceleration zone. The possible link of the variabilities to
thermal, dynamical and/or chemical processes within or under this region is
also discussed.
