Difference of photometric properties between regular and non-regular
  Miras in the Magellanic Clouds
  Mira variables are asymptotic giant branch pulsating stars with long
pulsation periods and large amplitudes in optical bands. By applying the random
forest algorithm to the I-band light curves for the Miras in the Magellanic
Clouds, we have classified these Miras into regular Miras and non-regular
Miras. Wherein non-regular Miras exhibit a long-term variation in addition to
their primary pulsation periods. Our results confirm that the period-luminosity
relation for maximum light has a smaller dispersion, but only occurs on the
regular oxygen-rich (O-rich) Miras, which we recommend to be applied in future
distance scale work. We have also collected multi-band photometry for these
Miras to perform a spectral-energy-distribution (SED) fitting with stellar and
dust components, showing that a significant fraction of dust is present around
the non-regular Miras. According to our results, we believe that the periodic
long-term variations seen in the non-regular Miras might be due to the presence
of dust.
