PIC simulations of reforming perpendicular shocks- implications for ion acceleration at SNRs and the heliospheric termination shock

Details PIC simulations of reforming perpendicular shocks- implications for ion acceleration at SNRs and the heliospheric termination shock PIC simulations of reforming perpendicular shocks- implications for ion acceleration at SNRs and the heliospheric termination shock

Dec 2004

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004agufmsh43a1085l&link_type=abstract

American Geophysical Union, Fall Meeting 2004, abstract #SH43A-1085

Astronomy and Astrophysics

Astrophysics

7807 Charged Particle Motion And Acceleration, 2104 Cosmic Rays, 2114 Energetic Particles, Heliospheric (7514), 2124 Heliopause And Solar Wind Termination, 3210 Modeling

Scientific paper

Recent particle-in-cell (PIC) simulations have revealed time-dependent shock solutions for parameters relevant to astrophysical and heliospheric shocks [e.g. 1,2,3]. These solutions are characterised by a shock which cyclically reforms on the spatio-temporal scales of the incoming protons. Whether a shock solution is stationary or reforming depends not only upon the model adopted for electron dynamics, but also on the plasma parameters, notably the upstream beta. For the heliospheric termination shock, these parameters are not well determined: some estimates suggest that the termination shock may be in a parameter regime such that it is time-dependent. It has been pointed out [3] that this may terminate some acceleration processes, for example shock surfing, which have been proposed for time-stationary shock solutions. The introduction of time-dependent electromagnetic fields intrinsic to the shock does however introduce the possibility of new mechanisms for the acceleration of protons. We will discuss the prospects for local ion acceleration at reforming quasiperpendicular shocks, in the presence of pickup ions as seen in selfconsistent PIC simulations with parameters relevant to both SNRs and the heliospheric termination shock. [1] Shimada, N., and M. Hoshino, Astrophys. J, 543, L67, 2000. [2] Schmitz, H., S.C. Chapman and R.O. Dendy, Astrophys. J, 570, 637, 2002 [3] Scholer, M., I. Shinohara and S. Matsukiyo, J. Geophys. Res., 108, 1014, 2003

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