Observations of He-4(++) ions in solar wind

Details Observations of He-4(++) ions in solar wind Observations of He-4(++) ions in solar wind

Jan 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994kosis..32...93y&link_type=abstract

Kosmicheskie Issledovaniya, vol. 32, p. 93

Physics

1

Solar Wind, Helium Ions, Solar Atmosphere, Interplanetary Medium, Solar Magnetic Field, Coronal Holes

Scientific paper

Results of a study of the characteristics of He-4(++) ions (alpha particles) in solar wind based on spaceborne measurements are summarized. The average helium abundance in solar wind is found to be lower than in the solar atmosphere and depends on the type of solar wind streams. High helium abundances are observed in plasma ejected from the solar atmosphere during nonstationary phenomena and also in flows from coronal hole type regions. Low helium abundances are observed in the heliospheric current sheet and in flows from coronal streamer type regions. It is suggested that processes responsible for the transfer of helium ions from the corona to the interplanetary medium are strongly dependent on the coronal magnetic field configuration.

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