  Coronal Mass Ejections (CMEs) are major drivers of extreme space weather
conditions, this being a matter of serious concern for our modern
technologically-dependent society. Development of numerical approaches that
would simulate CME generation and propagation through the interplanetary space
is an important step towards our capability to predict CME arrival times at
Earth and their geo-effectiveness. In this paper, we utilize a data-constrained
Gibson--Low (GL) flux rope model to generate CMEs. We derive the geometry of
the initial GL flux rope using the Graduated Cylindrical Shell (GCS) method.
This method uses multiple viewpoints from STEREO A & B Cor1/Cor2, and
SOHO/LASCO C2/C3 coronagraphs to determine the size and orientation of a CME
flux rope as it starts to erupt from the Sun. A flux rope generated in this way
is inserted into a quasi-steady global magnetohydrodynamics (MHD) background
solar wind flow driven by SDO/HMI line-of-sight magnetogram data, and erupts
immediately. Numerical results obtained with the Multi-Scale Fluid-Kinetic
Simulation Suite (MS-FLUKSS) code are compared with STEREO and SOHO/LASCO
coronagraph observations in particular in terms of the CME speed, acceleration,
and magnetic field structure.
