  An object with a very peculiar light-curve was discovered recently using
Kepler data. Authors argue that this object may be a transiting disintegrating
planet with a comet like dusty tail. We calculate the light-curves of stars
with such planets and take into account the Mie absorption and scattering on
spherical dust grains of various sizes assuming realistic dust opacities and
phase functions and finite radius of the source of the scattered light. The
planet light-curve is reanalysed using long and short cadence Kepler
observations from the first 14 quarters. Orbital period of the planet was
improved. We prove that the peculiar light-curve of this objects is in
agreement with the idea of a planet with a comet like tail. There is an
evidence of a quasi periodic long term evolution of the tail. Light-curve has a
prominent pre-transit brightening and a less prominent post-transit
brightening. Both are caused by the forward scattering and are a strong
function of the particle size. This feature enabled us to estimate a typical
particle size (radius) in the dust tail of about 0.1-1 micron. However, there
is an indication that the particle size changes along the tail. Larger
particles better reproduce the pre-transit brightening and transit core while
smaller particles are more compatible with the egress and post-transit
brightening. Dust density in the tail is a steep decreasing function of the
distance from the planet which indicates a significant tail destruction caused
by the star. We also argue that the 'planet' does not show uniform behaviour
but may have at least two constituents. This light-curve with pre-transit
brightening is analogous to the light-curve of $\epsilon$ Aur with mid-eclipse
brightening and forward scattering plays a significant role in such eclipsing
systems.
