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The most violent space weather events (eruptive solar flares and coronal massejections) are driven by the release of free magnetic energy stored in thesolar corona. Energy can build up on timescales of hours to days, and then maybe suddenly released in the form of a magnetic eruption, which then propagatesthrough interplanetary space, possibly impacting the Earth's space environment.Can we use the observed evolution of the magnetic and velocity fields in thesolar photosphere to model the evolution of the overlying solar coronal field,including the storage and release of magnetic energy in such eruptions? Theobjective of CGEM, the Coronal Global Evolutionary Model, funded by theNASA/NSF Space Weather Modeling program, is to develop and evaluate such amodel for the evolution of the coronal magnetic field. The evolving coronalmagnetic field can then be used as a starting point for magnetohydrodynamic(MHD) models of the corona, which can then be used to drive models ofheliospheric evolution and predictions of magnetic field and plasma densityconditions at 1AU.

The Coronal Global Evolutionary Model: Using HMI Vector Magnetogram and Doppler Data to Model the Buildup of Free Magnetic Energy in the Solar Corona