What Interplanetary Conditions Produce Quasi-Perpendicular Shocks?

Details What Interplanetary Conditions Produce Quasi-Perpendicular Shocks? What Interplanetary Conditions Produce Quasi-Perpendicular Shocks?

May 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008agusmsh43c..04r&link_type=abstract

American Geophysical Union, Spring Meeting 2008, abstract #SH43C-04

Physics

2111 Ejecta, Driver Gases, And Magnetic Clouds, 2114 Energetic Particles (7514), 2134 Interplanetary Magnetic Fields, 2139 Interplanetary Shocks

Scientific paper

The angle between the normal to an interplanetary shock front and the upstream magnetic field (θBn) is expected to influence the process of charged particle acceleration by the shock. Although θBn is often thought of as a property "of the shock", it also depends on the configuration of the interplanetary magnetic field (IMF) through which the shock is traveling. A typical, radially-propagating, CME-driven shock passing through a Parker spiral field at 1 AU would be expected to have θBn~45°; to produce a quasi-perpendicular shock (θBn~90°), the magnetic field direction must deviate significantly from the Parker spiral. We have investigated the solar wind context of a sample of near-Earth quasi-perpendicular shocks observed in solar cycle 23 and find that these shocks are frequently encountering interplanetary structures such as interplanetary coronal mass ejections (ICMEs), the heliospheric plasma sheet, or corotating interaction regions that are associated with significant deviations of the IMF direction. We also use Helios 1 and 2 magnetic field observations at 0.3-1 AU to examine how ICMEs may contribute to the formation of quasi-perpendicular shocks in the inner heliosphere.

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