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Upper limits for the solar wind He + content at 1 AU

1974; American Geophysical Union; Volume: 79; Issue: 13 Linguagem: Inglês

10.1029/ja079i013p01808

2156-2202

W. C. Feldman, J. R. Asbridge, S. J. Bame, P. D. Kearney,

Ionosphere and magnetosphere dynamics

Journal of Geophysical Research (1896-1977)Volume 79, Issue 13 p. 1808-1812 Upper limits for the solar wind He+ content at 1 AU W. C. Feldman, W. C. FeldmanSearch for more papers by this authorJ. R. Asbridge, J. R. AsbridgeSearch for more papers by this authorS. J. Bame, S. J. BameSearch for more papers by this authorP. D. Kearney, P. D. KearneySearch for more papers by this author W. C. Feldman, W. C. FeldmanSearch for more papers by this authorJ. R. Asbridge, J. R. AsbridgeSearch for more papers by this authorS. J. Bame, S. J. BameSearch for more papers by this authorP. D. Kearney, P. D. KearneySearch for more papers by this author First published: 1 May 1974 https://doi.org/10.1029/JA079i013p01808Citations: 26AboutPDF ToolsRequest permissionExport citationAdd to favoritesTrack citation ShareShare Give accessShare full text accessShare full-text accessPlease review our Terms and Conditions of Use and check box below to share full-text version of article.I have read and accept the Wiley Online Library Terms and Conditions of UseShareable LinkUse the link below to share a full-text version of this article with your friends and colleagues. Learn more.Copy URL Share a linkShare onEmailFacebookTwitterLinkedInRedditWechat Abstract An upper limit for the steady state solar wind He+ concentration is estimated from four Vela 5 and 6 heavy ion spectrums. The upper limit value for N(He+)/N(H) of 2.5 × 10−6 so obtained is at least an order of magnitude less than that predicted from presently accepted models of the local interstellar medium. The most likely explanation of the discrepancy is that wave-particle interactions are not capable of fully assimilating the initially non-Maxwellian high-temperature He+ particles of interstellar origin into the solar wind flow. Occasional flow conditions resulting in complete assimilation cannot be ruled out. References Asbridge, J. R., S. J. Bame, I. B. Strong, Outward flow of protons from the earth's bow shock, J. Geophys. Res., 73, 5777, 1968. Axford, W. I., The interaction of the solar wind with the interstellar medium, Solar WindNASA Spec. Publ. 308, 609, 1972. Axford, W. I., A. J. Dessler, R. Gottlieb, Termination of the solar wind and solar magnetic field, Astrophys. J., 137, 268, 1963. Bame, S. J., Spacecraft observations of the solar wind composition, Solar WindNASA Spec. Publ. 308, 535, 1972. Bame, S. J., A. J. Hundhausen, J. R. Asbridge, I. B. Strong, Solar wind ion composition, Phys. Rev. Lett., 20, 393, 1968. Bame, S. J., J. R. Asbridge, A. J. Hundhausen, M. D. 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