[P-EM10_29PM2] Wave, Turbulence, Reconnection, and Energetic Particles in Solar, Space and Laboratory

[PEM10-08] Acceleration and Diffusion of Cosmic Rays in Supernova Remnants in a Multi-Phase interstellar Medium

*Soonyoung ROH¹, Shu-ichiro INUTSUKA¹, Tsuyoshi INOUE² (1.Graduate School of Science, Nagoya University, 2.Department of Physics and Mathematics, Aoyama Gakuin University)

Keywords:Supernova Remnants, Diffusion of Cosmic Rays, Acceleration of Cosmic Rays, Pion-decay

Supernova remnants (SNRs) are one of the most powerful cosmic phenomena and are thought to be the dominant source of Galactic cosmic rays (CRs). A recent report by Funk et al. (2013) has shown an unequivocal signature of pion-decay in the gamma-ray spectra of SNRs. This provides strong evidence that high-energy protons are accelerated in SNRs. On the other hand, Fukui et al. (2012) showed that pion-decay from protons dominates in emission from SNR RX J1713 based on the spatial correlation of gamma-rays and molecular line emission. The actual gamma-ray emission from pion-decay should depend on the diffusion of CRs in a multi-phase interstellar medium with molecular clouds (Inoue et al. 2012). In order to quantitatively describe the diffusion of high energy CRs from acceleration sites, we have performed test particle numerical simulations using a three-dimensional magnetohydrodynamics (MHD) simulation data cube provided by Inoue et al. (2012). In this presentation, we analyze a realistic diffusion coefficient of cosmic rays in simulated SNRs, and discuss the possible implications for X-ray and gamma-ray observations.