Center for Space Environment Modeling Numerical Model of CME Initiation and Shock Development for the 1998 May 2 Event Ilia.

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Center for Space Environment Modeling Numerical Model of CME Initiation and Shock Development for the 1998 May 2 Event Ilia Roussev, Igor Sokolov, & Tamas Gombosi University of Michigan Terry Forbes & Marty Lee University of New Hampshire

Center for Space Environment Modeling Numerical Model & Results (from Roussev et al. 2004, ApJ, 605) Model: bOur model incorporates magnetogram data from Wilcox Solar Observatory and loss-of-equilibrium mechanism to initiate solar eruption. bEruption is achieved by slowly evolving boundary conditions for magnetic field to account for: Sunspot rotation; and Flux cancellation. Results: bExcess magnetic energy built in sheared field prior to eruption is 1.311x10 31 ergs; bFlux rope ejected during eruption achieves maximum speed in excess of 1,000 km/s; bCME-driven shock reaches fast-mode Mach number in excess of 4 and compression ratio greater than 3 at distance of 4R S from solar surface.

Center for Space Environment Modeling Dynamics of Solar Eruption

Center for Space Environment Modeling bCME-driven shock can develop close to Sun sufficiently strong to account for energetic solar protons up to a few GeV! bSEP acceleration by diffuse-shock-acceleration mechanism, up to energies sufficient for penetrating into spacecraft, occurs in Sun’s proximity at R~(3-12)R S and has relatively short time scale (~2 hrs). Conclusions

Center for Space Environment Modeling SEP Data for 1998 May 2 Event SEP Event (3-4)R S !

Center for Space Environment Modeling View of Eruption at t=3 hrs. Solid lines are magnetic field lines; false color code shows magnitude of current density. Flow speed is shown on translucent plane given by y=0. Values in excess of 1,000 km/s are blanked and shown in light grey. Inner sphere corresponds to R=R S ; color code shows distribution of radial magnetic field. Regions with radial field strength greater than 3 Gauss are blanked.