Modeling Quasar UV/Optical Variability with the Corona-heated
  Accretion-disk Reprocessing (CHAR) Model
  The rest-frame UV/optical variability of the quasars in the Sloan Digital Sky
Survey (SDSS) Stripe 82 is used to test the Corona-Heated Accretion-disk
Reprocessing (CHAR) model of Sun et al. 2020. We adopt our CHAR model and the
observed black-hole masses ($M_{\mathrm{BH}}$) and luminosities ($L$) to
generate mock light curves that share the same measurement noise and sampling
as the real observations. Without any fine-tuning, our CHAR model can
satisfactorily reproduce the observed ensemble structure functions for
different $M_{\mathrm{BH}}$, $L$, and rest-frame wavelengths. Our analyses
reveal that a luminosity-dependent bolometric correction is disfavored over the
constant bolometric correction for UV/optical luminosities. Our work
demonstrates the possibility of extracting quasar properties (e.g., the
bolometric correction or the dimensionless viscosity parameter) by comparing
the physical CHAR model with quasar light curves.
