  The optical emission of GRB 110205A is distinguished by two flares. In this
work we examine two possible scenarios for the optical afterglow emission. In
the first scenario, the first optical flare is the reverse shock emission of
the main outflow and the second one is powered by the prolonged activity of
central engine. We however find out that it is rather hard to interpret the
late ($t>0.1$ day) afterglow data reasonably unless the GRB efficiency is very
high ($\sim 0.95$). In the second scenario, the first optical flare is the low
energy prompt emission and the second one is the reverse shock of the initial
outflow. Within this scenario we can interpret the late afterglow emission
self-consistently. The reverse shock region may be weakly magnetized and the
decline of the second optical flare may be dominated by the high latitude
emission, for which strong polarization evolution accompanying the quick
decline is possible, as suggested by Fan et al. in 2008. Time-resolved
polarimetry by RINGO2-like polarimeters will test our prediction directly.
