  We present detailed broadband X-ray spectral variability of a Seyfert 1
galaxy 1H~0419--577 based on an archival \suzaku{} observation in July 2007, a
new \suzaku{} observation performed in January 2010 and the two latest \xmm{}
observations from May 2010. All the observations show soft X-ray excess
emission below $2\kev$ and both \suzaku{} observations show a hard X-ray excess
emission above $10\kev$ when compared to a power-law. We have tested three
physical models -- a complex partial covering absorption model, a blurred
reflection model and an intrinsic disk Comptonization model. Among these three
models, the blurred reflection model provided statistically the best-fit to all
the four observations. Irrespective of the models used, the soft X-ray excess
emission requires contribution from a thermal component similar to that
expected from an accretion disk. The partial covering absorption model results
in a nonphysical high temperature ($kT_{in} \sim 100\ev$) for an accretion disk
and is also statistically the worst fit among the three models. 1H~0419--577
showed remarkable X-ray spectral variability. The soft X-ray excess and the
power-law both became weaker in January 2010 as well as in May 2010. A
moderately broad iron line, detected in July 2007, is absent in the January
2010 observation. Correlated variability of the soft X-ray excess and the iron
$K\alpha$ line strongly suggest reflection origin for both the components.
However, such spectral variability cannot be explained by the light bending
model alone and requires changes in the accretion disk/corona geometry possibly
arising from changes in the accretion rate.
