Counterstreaming solar wind halo electron events - Solar cycle variations

Details Counterstreaming solar wind halo electron events - Solar cycle variations Counterstreaming solar wind halo electron events - Solar cycle variations

May 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992jgr....97.6531g&link_type=abstract

Journal of Geophysical Research (ISSN 0148-0227), vol. 97, no. A5, May 1, 1992, p. 6531-6535. Research supported by DOE.

Physics

48

Solar Electrons, Solar Wind, Stellar Mass Ejection, Sunspot Cycle, Halos, Solar Activity Effects, Solar Corona

Scientific paper

It is shown that during the interval from August 1978 through December 1990 the frequency of the occurrence of counterstreaming events varied roughly in phase and amplitude with coronal mass ejecta (CME) rates derived from coronagraph observations and with the advance of the solar activity cycle as measured, e.g., by sunspot numbers. It is inferred that CMEs in the solar wind near 1 AU can usually be identified by the counterstreaming solar wind halo electron signature.

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