Time-series analyses of Cepheid and RR Lyrae variables in the wide-field
  variability surveys
  We discuss time-series analyses of classical Cepheid and RR Lyrae variables
in the Galaxy and the Magellanic Clouds at multiple wavelengths. We adopt the
Fourier decomposition method to quantify the structural changes in the light
curves of Cepheid and RR Lyrae variables. A quantitative comparison of Cepheid
Fourier parameters suggests that the canonical mass-luminosity models that lie
towards the red-edge of the instability strip show a greater offset with
respect to observations for short-period Cepheids. RR Lyrae models are
consistent with observations in most period bins. We use ensemble light curve
analysis to predict the physical parameters of observed Cepheid and RR Lyrae
variables using machine learning methods. Our preliminary results suggest that
the posterior distributions of mass, luminosity, temperature and radius for
Cepheids and RR Lyraes can be well-constrained for a given metal abundance,
provided a smoother grid of models is adopted in various input physical
parameters.
