Physics
Scientific paper
Dec 2010
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010agufmsh33c..06t&link_type=abstract
American Geophysical Union, Fall Meeting 2010, abstract #SH33C-06
Physics
[2102] Interplanetary Physics / Corotating Streams, [2109] Interplanetary Physics / Discontinuities, [2139] Interplanetary Physics / Interplanetary Shocks, [2164] Interplanetary Physics / Solar Wind Plasma
Scientific paper
One dimensional hybrid simulations are performed to investigate the energetics occurring around the corotating interaction regions (CIRs). A pair of shocks bounding the CIRs are one of the major sources responsible for the particle acceleration in the heliosphere. The nature of heating/acceleration at the forward (FS) and reverse (RS) shocks is distinguished in detail. The FS accelerates the slow solar wind and produces more energetic particles than the RS, where the fast solar wind is decelerated. One prominent feature is that the leakage of energetic particles is taken place in the upstream of FS as the CIR evolution proceeds. This might imply that the FS can not retain its strength due to the effect of solar wind expansion. In the region between the RS and the streaming interface (SI), where the fast solar wind is the dominant component, the effect of the presence of large-amplitude rotational Alfvenic field is demonstrated. The result exhibits the formation of magnetic decreases (MDs), which give a localized reduction in the magnetic field. In the present model, the mechanism of MD formation is explicable in terms of the temperature anisotropy relaxation by the imposed Alfvenic fluctuations. Large pitch-angle scattering is subsequently taken place, leading to the stronger thermalization. Also shown is that the MD is hardly transmitted to the slow solar wind region over the SI, supporting the observations that the MD clusters were dominantly identified in the trailing portions of CIRs (Tsurutani et al., 2009).
Kubo Yoshio
Tsubouchi Ken
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