On the sources of interplanetary shocks at 0.72 AU

Details On the sources of interplanetary shocks at 0.72 AU On the sources of interplanetary shocks at 0.72 AU

Jan 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994jgr....99...11l&link_type=abstract

Journal of Geophysical Research (ISSN 0148-0227), vol. 99, no. A1, p. 11-17

Physics

43

Interplanetary Magnetic Fields, Plasma Density, Plasma Temperature, Shock Waves, Solar Corona, Ion Temperature, Solar Cycles, Statistical Analysis, Stellar Mass Ejection

Scientific paper

In order to understand the solar cycle variation of interplanetary shocks and their driving source at 0.72 AU, a survey of Pioneer Venus Orbiter (PVO) magnetometer and plasma data from 1979-1988 has been conducted. Known shock drivers at 1.0 AU include coronal mass ejections (CMEs) and fast/slow stream interactions. In our analysis, CMEs were identified by a decrease in plasma temperature to background or below accompanied by an increase in plasma density and dynamic pressure. It was also required that the magnetic field exhibit a coherent rotation over about a day and an increase and decline in magnitude on a timescale of hours to days. Stream interactions were identified by a characteristic increase in ion temperature and velocity coincident with a decrease in density and a coincident increase in the total magnetic field magnitude. These signatures were usually preceded within 24 hours by a change in flow angle. In all, 45 shocks were identified: 36 driven by CMEs, 6 resulting from fast/slow stream interactions, and 3 with sources that could not be defined. The shocks driven by CMEs show a solar cycle variation that roughly follows the sunspot number. These shocks all have normals consistent with radial propagation of the shock fronts from the sun. In contrast, the few stream interaction related shocks show a tendency to occur later in the solar cycle and have a broader distribution of shock normals.

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