  We present the multi-wavelength observations of asymmetric filament eruption,
associated CME and coronal downflows on 2012 June 17-18 during 20:00-05:00 UT.
We use SDO/AIA, STEREO-B/SECCHI observations to understand the filament
eruption scenario and its kinematics. While LASCO C2 observations have been
analyzed to study the kinematics of the CME and associated downflows. SDO/AIA
limb observations show that the filament exhibits whipping like asymmetric
eruption. STEREO/EUVI disk observations reveal a two ribbon flare underneath
the south-eastern part of the filament that is most probably occurred due to
reconnection process in the coronal magnetic field in the wake of the filament
eruption. The whipping like filament eruption later gives a slow CME in which
the leading edge and the core propagate respectively with the average speed of
$\approx$ 540 km s$^{-1}$ and $\approx$ 126 km s$^{-1}$ as observed in the
LASCO C2 coronagraph. The CME core formed by the eruptive flux-rope shows the
outer coronal downflows with the average speed of $\approx$ 56 km s$^{-1}$
after reaching up to $\approx$4.33 $R_{\sun}$. Initially, the core decelerates
with $\approx$ 48 m s$^{-2}$. The plasma first decelerates gradually up to the
height of $\approx$4.33 $ R_{\sun}$ and then starts accelerating downward. We
suggest a self-consistent model of a magnetic flux rope representing the
magnetic structure of the CME core formed by eruptive filament that lost its
previous stable equilibrium when reach at a critical height. With some
reasonable parameters, and inherent physical conditions the model describes the
non-radial ascending motion of the flux rope in the corona, its stopping at
some height, and thereafter the downward motion, which are in good agreement
with the observations.
