Fig. A.1.

Download original image
In situ observation of the ICME resulting from the 2011 October 22 solar event. Shown from top to bottom are the magnetic field magnitude B, field inclination angle θ (with respect to the ecliptic plane), azimuthal angle ϕ (0 deg pointing to the Sun), three components (Vx, Vy, Vz) of the solar wind velocity in the GSE coordinate system, proton density Np, proton temperature Tp (superimposed by Tp/Texp, where Texp is an empirical temperature determined from solar wind speed), plasma β, and half of the field-line length assuming that the flux-rope axial length is in the range 2–π AU. The dashed red curves show the model fitting results with the uniformly twisted flux-rope (Gold-Hoyle) solution. The closest approach of the observational path to the flux-rope axis d is 0.37 in terms of the rope radius; the goodness of fit χn is 0.21, which is the normalized root mean square of the difference between the fitting and observation.
Current usage metrics show cumulative count of Article Views (full-text article views including HTML views, PDF and ePub downloads, according to the available data) and Abstracts Views on Vision4Press platform.
Data correspond to usage on the plateform after 2015. The current usage metrics is available 48-96 hours after online publication and is updated daily on week days.
Initial download of the metrics may take a while.