Abstract
The theory that most, if not all, interplanetary shocks are caused by coronal mass ejections (CMEs) faces serious problems in accounting for the strongest shocks. The difficulties include (i) a remarkable absence of very strong shocks during solar maximum 1980 when CMEs were prolific, (ii) unrealistic initial speeds near the Sun for impulsive models, (iii) the absence of rarefaction zones behind the shocks and (iv) sustained high speed flows following shocks which are not easily explained as consequences of CME eruptions. Observations of the proton temperature near 1 AU indicate that strong shock drivers have properties similar to high speed streams emitted by coronal holes. Eruptions of fast solar wind from coronal holes influenced by solar activity can explain the occurrence of the strongest interplanetary shocks.
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Borrini, G., Gosling, J.T., Barnes, S.J., and Feldman, W.C.: 1982,J. Geophys. Res.,87, 4365.
Kahler, S.W.: 1992,Annu. Rev. Astron. Astrophys.,30, 113.
Webb, D.F. and Howard, R.A.: 1994,J. Geophys. Res.,99, 4201.
Krivsky, L., Gopasyuk, S., and Soliman, M.A.: 1992,Publications Astr. Inst. Czechosl. No. 80.
Couzens, D.A. and King, J.H.: 1986, Interplanetary medium data book, supplement 3A NSSDC/WDC-A-R&S 86-04,Natl. Space Sci. Data Cent. Greenbelt, MD.
Thompson, R.: 1990,Proceedings of Solar-Terrestrial Predictions Workshop, Leura, Australia Oct 16–20, 1989, Vol1, 598.
Smith, Z., and Dryer, M.: 1991,Solar Phys.,131, 363
Smith, Z., and Dryer, M.: 1990,Solar Phys.,129, 387
Kahler, S.W. and Hundhausen, A.J.: 1992,J. Geophys. Res.,97, 1619
Bravo, S., and Perez-Enriquez, R.: 1994,Rev. Mexicana de Astr. y Astrophys.,28, 17.
Hewish, A., Tappin, S.J. and Gapper, G.R.: 1985,Nature,314, 137.
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Hewish, A. Low density drivers of strong interplanetary shocks. Astrophys Space Sci 243, 5–13 (1996). https://doi.org/10.1007/BF00644026
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DOI: https://doi.org/10.1007/BF00644026