Nonlinear Alfvén waves in high-speed solar wind streams
1977; American Geophysical Union; Volume: 82; Issue: 4 Linguagem: Inglês
10.1029/ja082i004p00618
ISSN2156-2202
AutoresBarbara Abraham‐Shrauner, W. C. Feldman,
Tópico(s)Astro and Planetary Science
ResumoJournal of Geophysical Research (1896-1977)Volume 82, Issue 4 p. 618-624 Nonlinear Alfvén waves in high-speed solar wind streams B. Abraham-Shrauner, B. Abraham-ShraunerSearch for more papers by this authorW. C. Feldman, W. C. FeldmanSearch for more papers by this author B. Abraham-Shrauner, B. Abraham-ShraunerSearch for more papers by this authorW. C. Feldman, W. C. FeldmanSearch for more papers by this author First published: 1 February 1977 https://doi.org/10.1029/JA082i004p00618Citations: 57AboutPDF 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 A nonlinear proton distribution function that is an exact stationary solution of the nonlinear Vlasov equation and Maxwell's equations and which supports a single nonlinear transverse Alfvén (ion cyclotron) wave that is circularly polarized and nondispersive is proposed for most of the observations during high-speed solar wind streams. This nonlinear distribution removes the strong Alfvén wave instability, inconsistent with the persistence of the observed proton distribution functions in high-speed streams, found by the linear stability analysis. Model temperature anisotropies and drift velocities of the two spatially inhomogeneous bi-Maxwellian components are consistent with typical proton velocity distributions measured in high-speed streams at 1 AU. Two derived relations for each of the wave number and the phase velocity of the wave are obeyed within experimental uncertainties by two typical proton measurements. Our model also predicts that the alpha particle bulk flow velocity exceeds the proton particle bulk flow velocity, as is observed. References Abraham-Shrauner, B., Exact, stationary wave solutions of the nonlinear Vlasov equation, Phys. Fluids, 11, 1162, 1968. Asbridge, J. R., S. J. Bame, W. C. Feldman, M. D. Montgomery, Helium and hydrogen velocity differences in the solar wind, J. Geophys. Res., 81, 2719, 1976. Bame, S. J., J. R. Asbridge, W. C. Feldman, S. P. Gary, M. D. Montgomery, Evidence for local ion heating in solar wind high speed streams, Geophys. Res. Lett., 2, 373, 1975. Barnes, A., J. V. Hollweg, Large-amplitude hydromagnetic waves, J. Geophys. Res., 79, 2302, 1974. Behannon, K. W., Observations of electromagnetic waves in IMF between 1 and 0.46 AU (abstract), Eos Trans. AGU, 57, 319, 1976. Berger, R. L., R. 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