All Figures

$\begin{figure} \par\includegraphics[width=8.2cm,clip]{4806fig_1.eps}\end{figure}$ Figure 1: Wind observations for the magnetic cloud observed on 18-20 October, 1995 (one minute cadence). From the upper to the lower panel: radial ( $B_{x, \rm cloud}$ ), azimuthal ( $B_{y, \rm cloud}$ ), and axial ( $B_{z, \rm cloud}$ ) components of the magnetic field (local coordinates, as deduced from the MV), bulk velocity (V), and proton density ( $n_{\rm p}$ ), as a function of time (in hours, after 00:00 UT, October 18, 1995). Dashed lines mark the front boundary of the cloud (18:58 UT, October 18, 1995). Between dash-dotted lines we mark the range of possible ends of the cloud (October 19, 22:54 UT and October 20, 01:38 UT).
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In the text

$\begin{figure} \par\includegraphics[width=7.9cm,clip]{4806fig_2.eps}\end{figure}$ Figure 2: Axial component, $B_{z, \rm cloud}$ , of the cloud magnetic field (local coordinate system from MV) as a function of time (in hours, after 18:58 UT, October 18, 1995). Dots correspond to the observed field (temporal cadence of one minute), solid line to the Lundquist model, dashed line to the Gold-Hoyle model, dotted line to the Hidalgo model and dash-dotted line to the Cid model.
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In the text

$\begin{figure} \par\includegraphics[width=7.9cm,clip]{4806fig_3.eps}\end{figure}$ Figure 3: Field component in the direction orthogonal to both the spacecraft trajectory and the MC axis. $B_{y, \rm cloud}$ is the azimuthal component of the magnetic field with the hypothesis of negligible impact parameter. The plotting convention is the same as in Fig. 2.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{4806fig_4.eps}\end{figure}$ Figure 4: Axial magnetic field (B₀), axial twist per unit length ( $\tau _0$ ), fluxes ( $F_\phi /L$ and F_z) and helicity (H/L), for the different chosen end times, as a function of the corresponding estimated MC radius R (see Sect. 4.6). Asterisks and solid line correspond to model L, triangles and dashed line to model G, X-symbol and the dotted line to model H, the O-symbol and dot-dashed line to model C. The vertical dashed line shows the end boundary of the magnetic cloud set on October 19, 22:54 UT. The radius range corresponds to the 21 equi-spaced end boundaries chosen between October 19, 17:31 UT and October 20, 01:38 UT.
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In the text

$\begin{figure} \par\includegraphics[width=7.8cm,clip]{4806fig_5.eps}\end{figure}$ Figure 5: Accumulative flux of $B_{y, \rm cloud}$ (thick solid line) starting from the leading boundary of the cloud. Thin solid line shows $B_{y, \rm cloud}$ as a reference (in arbitrary units). The times of minimum and null flux accumulation are marked with vertical dashed lines.
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In the text

$\begin{figure} \par\hspace*{-1.2cm} \includegraphics[width=7cm,clip]{4806fig_6a.eps}\vspace*{2mm} \includegraphics[width=6cm,clip]{4806fig_6b.eps}\end{figure}$ Figure 6: Schematic 2D view of the magnetic cloud embedded in the solar wind near the Sun ( top) and during the spacecraft passage at 1 AU ( bottom). Because the MC is faster than the surrounding solar wind and their magnetic fields form a large angle (anti-parallel in the scheme), reconnection is forced in front of the MC (see Sect. 5.2). The horizontal dashed line in the bottom figure indicates the spacecraft trajectory.
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In the text

$\begin{figure} \par\includegraphics[width=7.8cm,clip]{4806fig_7.eps}\end{figure}$ Figure 7: Accumulative azimuthal flux per unit length ( $F_{y,e} /L \approx F_{\phi ,e} /L$ , in 10²¹ Mx/AU), axial flux (F_z,e, in 10²¹ Mx), and magnetic helicity per unit length (H_e/L, in 10⁴² Mx²/AU), as function of |x| where x is the coordinate along the projection of the spacecraft trajectory orthogonal to the MC axis. The location of the MC centre was chosen at 07:26 UT on October 19 (Sect. 5.1). The solid vertical line shows the position of the front of the MC (at $x=X_{\rm in}$ ) and the dotted vertical line the position of the rear boundary (at $x=X_{\rm out}$ ) selected to have flux balance in $B_{y, \rm cloud}$ . The dashed vertical line shows the position of the back of the MC (at $x=X_{\rm back}$ ).
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In the text

$\begin{figure} \par\includegraphics[width=7.9cm,clip]{4806fig_2.eps}\end{figure}$	Figure 2: Axial component, $B_{z, \rm cloud}$ , of the cloud magnetic field (local coordinate system from MV) as a function of time (in hours, after 18:58 UT, October 18, 1995). Dots correspond to the observed field (temporal cadence of one minute), solid line to the Lundquist model, dashed line to the Gold-Hoyle model, dotted line to the Hidalgo model and dash-dotted line to the Cid model.
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$\begin{figure} \par\includegraphics[width=7.9cm,clip]{4806fig_3.eps}\end{figure}$	Figure 3: Field component in the direction orthogonal to both the spacecraft trajectory and the MC axis. $B_{y, \rm cloud}$ is the azimuthal component of the magnetic field with the hypothesis of negligible impact parameter. The plotting convention is the same as in Fig. 2.
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$\begin{figure} \par\includegraphics[width=7.8cm,clip]{4806fig_5.eps}\end{figure}$	Figure 5: Accumulative flux of $B_{y, \rm cloud}$ (thick solid line) starting from the leading boundary of the cloud. Thin solid line shows $B_{y, \rm cloud}$ as a reference (in arbitrary units). The times of minimum and null flux accumulation are marked with vertical dashed lines.
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