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Predictions of the arrival time of Coronal Mass Ejections at 1AU: an analysis of the causes of errors

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Academic year: 2017

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Fig. 2. The transit time of a CME to 1 AU as a function of the CME speed for the 35 E-S line events
Table 2. Comparison of models with the observations of the 35 E-S line CMEs.
Fig. 4. The difference between the predicted and observed transit times to 1 AU (1τ) against solar wind speed upstream of the ICME.
Fig. 5. The average magnetic field intensity of an ICME as a func- func-tion of 1τ (predicted – actual τ )
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