  The traditional cone models achieve great success in studying the geometrical
and kinematic properties of halo coronal mass ejections (CMEs). In this paper,
a revised cone model is proposed to investigate the properties of CMEs as a
result of non-radial prominence eruptions. The cone apex is located at the
source region of an eruption instead of the Sun center. The cone axis deviates
from the local vertical by an inclination angle of $\theta_1$ and an angle of
$\phi_1$. The length and angular width of the cone are $r$ and $\omega$,
respectively. The model is successfully applied to two CMEs originating from
the western limb on 2011 August 11 and 2012 December 7. By comparing the
projections of the cones with the CME fronts simultaneously observed by the
Atmospheric Imaging Assembly (AIA) on board the Solar Dynamics Observatory
(SDO) and the Extreme-Ultraviolet Imager (EUVI) on board the ahead Solar
TErrestrial RElations Observatory (STEREO), the properties of the CMEs are
derived, including the distance, angular width, inclination angle, deviation
from the plane of the sky, and true speed in space. This revised cone model
provides a new and complementary approach in exploring the whole evolutions of
CMEs.
