Modeling suprathermal proton acceleration by an ICME within 0.5 AU: the May 13, 2005 event K. A. Kozarev 1,5 R. M. Evans 2, M. A. Dayeh 3, N. A. Schwadron 4, M. Opher 2, K. E. Korreck 5, and T. I. Gombosi 6 1 Boston University, Boston, MA; 2 George Mason University, Fairfax, VA; 3 Southwest Research Institute, San Antonio, TX; 4 University of New Hampshire, Durham, NH; 5 Smithsonian Astrophysical Observatory, Cambridge, MA; 6 University of Michigan, Ann Arbor, MI We modeled the acceleration of suprathermal protons to high energies by a complex traveling plasma structure between AU. We used a global 3D MHD simulation of the May 13, 2005 coronal mass ejection event, and coupled it to a global kinetic code for particle acceleration and propagation. We scaled pre-event suprathermal spectra observed at 1 AU to 2.5 Rs and used them for inner boundary conditions for the kinetic simulation. We find that suprathermal protons can become the seed for solar energetic particles, as they get strongly energized by the enhanced traveling shock and complex plasma structure in the corona and interplanetary space. The kinetic model The Energetic Particles Radiation Environment Module (EPREM; Schwadron et al. 2010, Kozarev et al. 2010) solves numerically the focused transport equation (Kota et al., 2005) on a dynamical grid representing the inner heliosphere, in which nodes are convected outward from the sun according to the underlying solar wind parameters. This parallelized code solves for streaming, adiabatic cooling and focusing, convection, pitch-angle scattering, and stochastic acceleration effects. Energetic particles are accelerated and transported through this grid along magnetic field lines, based on interplanetary conditions. Coupling between kinetic and MHD models We extracted a 3D box (100x100x100 cells) around the expanding CME in the MHD simulation at two-minute increments (shown in Fig. 2). The kinetic code does trilinear interpolation on the BATSRUS box to obtain plasma parameters. Outside the box we extrapolate, assuming a constant solar wind speed, and an inverse square radial dependence of density and magnetic field. Modeling the May 13, 2010 event The EPREM simulation radial domain is between 2.5 Rs and 0.6 AU. We set up a computational grid dense enough close to the sun to resolve the features in the plasma model, that becomes sparse beyond 0.1 AU. The energy range of the injected proton spectra was between MeV. We use a fixed particle mean free path of 0.1 AU, consistent with the particle energies. Following Dayeh et al. (2009), we use quiet time He-4 ion (0.1 – 0.5 MeV/nuc) observations from ACE/ULEIS at L1 to obtain a seed suprathermal proton pre-event spectrum of the form dJ/dE=9.95 x x E We convert the spectrum to protons at 10 Rs assuming: 1) the flux is scaled to 2.5 Rs via an inverse-square dependence; 2) a helium to proton abundance of 10%; 3) the resulting spectral form is valid between Mev. We inject the scaled spectrum uniformly at the inner boundary of the kinetic code. The simulation spans half a day of data time. Summary and Future Work We have combined results from a time-dependent global MHD simulation of the May 13, 2005 coronal mass ejection with a global kinetic code, and modeled proton acceleration and transport between 2.5 solar radii and 0.5 AU, for energies MeV. We used a quiet time suprathermal Helium-4 spectrum observed at 1 AU and scaled to represent protons in the solar corona. We find that the suprathermal particles are easily energized by the transient plasma structure, and could serve as the seed population for solar energetic particles created by strong interplanetary shocks. In future work we will expand our simulations to 1 AU in order to verify our simulations against observations, and further refine them. We are also improving the integration of MHD simulation results in order to cover the entire kinetic code domain. Introduction Coronal Mass Ejection (CME)-driven interplanetary shocks are able to accelerate charged particles to high energies, potentially dangerous to astronauts and spacecraft electronics. This is an important problem in heliospheric physics, space weather forecasting and space operations. Recent modeling work has shown that interplanetary shocks can be very effective in accelerating particles up to several GeV/nuc close to the sun, but are not very efficient as they move outward (Zank et al., 2000; Roussev et al., 2004). We investigate how quiet-time suprathermal protons close to the sun can become the seed population for energetic protons accelerated by a complex traveling plasma structure in the solar corona, and transported in the inner heliosphere. We have simulated the May 13, 2005 CME event with a global 3D MHD and coupled it to a kinetic model. References Altschuler, M. D. & Newkirk, G., 1969, Sol. Phys., 9, 131 Powell, K. G. et al., 1999, J. Comp. Phys., 154, 284 Arge, C. N. & Pizzo, V. J., 2000, J. Geophys. Res., 105, A5 Roussev, I. I. et al., 2004, ApJ., 605, L73 Cohen, O., et al., 2007, ApJ, 654, L163 Schwadron, N. A. et al., 2006, IEEEAC Paper #1001, 6 Cohen, O. et al., 2008, J. Geophys. Res., 113, A03104 Schwadron, N. A. et al., 2010, Space Weather, 8, 10 Dayeh, M. A. et al., 2009, Astrophys. J., 693, 1588 Thompson, B. J. et al., 1998, Geophys. Res. Lett., 25, 14, 2465 Kota, J. et al., 2005, The Physics of Collisionless shocks, AIP Toth, G. et al., 2005, J. Geophys. Res., 110, A12226 Kozarev, K. et al., 2010, Space Weather, 8, 10 Zank, G. P. et al, 2000, J. Geophys. Res., 105, A11 Fig. 2. EPREM's dynamic grid shown near the origin. Red dots represent grid nodes, streamlines are traced in white. The green box shows the region containing the expanding CME structure. Fig.3 Average shock properties as a function of distance. The shock remained very strong between 2 and 20 solar radii. Fig. 5. Modeled proton fluxes over four hours at 0.5 AU for energies MeV (left) and MeV (right). The time-dependent behavior is caused by the traveling shock and plasma structure. The MHD model We use the Space Weather Modeling Framework (Toth et al. 2005) for modeling the global solar wind and CME. The 3D magnetohydrodynamic (MHD) code Block Adaptive Tree Solar-Wind Roe Upwind Scheme (BATS-R-US) which serves as its core is highly parallelized and includes adaptive mesh refinement. The initial solar magnetic field is calculated with the Potential Field Source Surface model (Altschuler & Newkirk. 1969) and an MDI synoptic magnetogram for CR 2029 (corresponding to April-May 2005.)‏ After steady-state is achieved, grid resolution in the CME region is increased in order to capture the shock and ICME properties. A modified Titov-Demoulin (TD) flux rope (Roussev et al. 2004) is inserted out of equilibrium in an active region near the equator. The ejecta field is poloidal. The flux rope's magnetic field orientation is anti-parallel to the active region magnetic field, and perpendicular to the global coronal field. The initial free energy is 2 x ergs. Fig.1. Density contour plot of the CME and solar magnetic field. The red square shows the approximate size and position of the box extracted from the MHD model, for this particular time step. Fig.4. Event fluence at 0.3 and 0.5 AU, between MeV, compared with the source spectrum at 0.15 AU (black).