On the Origin of the Dramatic Spectral Variability of WPVS 007
  We report the discovery of large-amplitude mid-infrared variabilities (MIR;
$\sim 0.3$ mag) in the Wide-field Infrared Survey Explorer W1 and W2 bands of
the low-luminosity narrow-line Seyfert 1 galaxy WPVS 007, which exhibits
prominent and varying broad-absorption lines (BALs) with blueshifted velocity
up to $\rm \sim 14000\ km\ s^{-1}$. The observed significant MIR variability,
the UV to optical color variabilities in the Swift bands that deviate from the
predictions of pure dust attenuation models, and the fact that Swift light
curves can be well fitted by the stochastic AGN variability model suggest that
its observed flux variabilities in UV-optical-MIR bands should be intrinsic,
rather than owing to variable dust extinction. Furthermore, the variations of
BAL features (i.e., trough strength and maximum velocity) and continuum
luminosity are concordant. Therefore, we propose that the BAL variability
observed in WPVS 007 is likely induced by the intrinsic ionizing continuum
variation, alternative to the rotating-torus model proposed in a previous work.
The BAL gas in WPVS 007 might be in the low-ionization state as traced by its
weak N V BAL feature; as the ionizing continuum strengthens, the Ci IV and Si
IV column densities also increase, resulting in stronger BALs and the emergence
of high-velocity components of the outflow. The outflow launch radius might be
as small as $\sim 8 \times 10^{-4}$ pc under the assumption of being
radiatively driven, but a large-scale origin (e.g., torus) cannot be fully
excluded because of the unknown effects from additional factors, e.g., the
magnetic field.
