Acceleration of Anomalous Cosmic Rays at a Blunt Termination Shock with Varying Strength along the Shock Face

Details Acceleration of Anomalous Cosmic Rays at a Blunt Termination Shock with Varying Strength along the Shock Face Acceleration of Anomalous Cosmic Rays at a Blunt Termination Shock with Varying Strength along the Shock Face

Dec 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008agufmsh13c..06k&link_type=abstract

American Geophysical Union, Fall Meeting 2008, abstract #SH13C-06

Physics

2104 Cosmic Rays, 2134 Interplanetary Magnetic Fields, 2144 Interstellar Gas, 7845 Particle Acceleration

Scientific paper

Voyagers' crossing of the termination shock (TS) in 2004 and 2007 brought several surprises. The spectrum of anomalous cosmic rays (ACRs) did not unfold to a smooth power law at the shock. ACR fluxes continued to increase into the heliosheath and ACR spectra seen by V-1 unfolded gradually. The recent observation of Stereo, indicating a double peak in the flux of energetic neutral atoms (ENAs) (Wang et al., Nature, 454, p 81, 2008) poses further challenge for theoretical modelers. We consider a two-dimensional model of the global heliosphere with an offset circle representing the blunt termination shock. Field lines wound in a Parker spiral cross the TS multiple times. Parker's diffusive transport equation is solved including anisotropic diffusion, convection adiabatic cooling and shock acceleration. In our earlier simulations we assumed the same strength everywhere along the shock. It is quite likely, however, that the TS is stronger at the nose region and less strong toward the flanks and tail, rendering acceleration less effective at the flanks and tail. We present numerical simulation results and discuss implications.

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