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We perform and analyze results of a global magnetohydrodyanmic (MHD)simulation of the fast coronal mass ejection (CME) that occurred on 2011 March7. The simulation is made using the newly developed Alfv\'en Wave Solar Model(AWSoM), which describes the background solar wind starting from the upperchromosphere and extends to 24 R$_{\odot}$. Coupling AWSoM to an innerheliosphere (IH) model with the Space Weather Modeling Framework (SWMF) extendsthe total domain beyond the orbit of Earth. Physical processes included in themodel are multi-species thermodynamics, electron heat conduction (bothcollisional and collisionless formulations), optically thin radiative cooling,and Alfv\'en-wave turbulence that accelerates and heats the solar wind. TheAlfv\'en-wave description is physically self-consistent, includingnon-Wentzel-Kramers-Brillouin (WKB) reflection and physics-based apportioningof turbulent dissipative heating to both electrons and protons. Within thismodel, we initiate the CME by using the Gibson-Low (GL) analytical flux ropemodel and follow its evolution for days, in which time it propagates beyondSTEREO A. A detailed comparison study is performed using remote as well as\textit{in situ} observations. Although the flux rope structure is not compareddirectly due to lack of relevant ejecta observation at 1 AU in this event, ourresults show that the new model can reproduce many of the observed featuresnear the Sun (e.g., CME-driven extreme ultraviolet (EUV) waves, deflection ofthe flux rope from the coronal hole, "double-front" in the white light images)and in the heliosphere (e.g., shock propagation direction, shock properties atSTEREO A).

Chromosphere to 1 AU Simulation of the 2011 March 7th Event: A Comprehensive Study of Coronal Mass Ejection Propagation