Control of Suprathermal Electron Flux by Solar Wind Dynamics

Physics

Scientific paper

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2102 Corotating Streams, 2114 Energetic Particles (7514), 2134 Interplanetary Magnetic Fields, 2164 Solar Wind Plasma

Scientific paper

The high variability of the intensity of suprathermal electron flux in the solar wind is usually ascribed to the high variability of sources on the Sun. Here we demonstrate that a substantial amount of the variability arises instead from solar wind dynamics in stream interaction regions, where fast wind runs into slow wind and creates a pressure ridge at the interface. Superposed epoch analysis centered on stream interfaces in 26 interaction regions previously identified in Wind data reveal a twofold increase in 250-eV flux (integrated over pitch angle). This result is understood in terms of the magnetic field compression there. If suprathermal electrons spiraling along field lines are viewed as beads along strings, then increasing the density of the strings through compression will also increase the density of the beads. An intriguing aspect of the result is that while the field strength peaks at the stream interface, as expected, the peak in electron flux lags by ˜1.5 hours. Although this lag may not be statistically significant, its sense is consistent with the systematic transport of open magnetic flux via interchange reconnection at coronal hole boundaries predicted by the global footpoint circulation model of L. A. Fisk and colleagues.

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