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![(a) Time series of primarily proton (p + ) flux at >1 MeV, (b) H+ flux around 30-500 keV, (c) solar wind density and (d) radial speed, (e) magnetic field vector and magnitude over interval c. (f)-(h) Magnification of the dispersive SEP event and CME for H+ flux around 30-500 keV. From [28].](profile/O-Malandraki/publication/358625990/figure/fig3/AS:1171903951712257@1656415083549/a-Time-series-of-primarily-proton-p-flux-at-1-MeV-b-H-flux-around-30-500-keV.png)
(a) Time series of primarily proton (p + ) flux at >1 MeV, (b) H+ flux around 30-500 keV, (c) solar wind density and (d) radial speed, (e) magnetic field vector and magnitude over interval c. (f)-(h) Magnification of the dispersive SEP event and CME for H+ flux around 30-500 keV. From [28].
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