Table 2: Geometrical (obtained from the minimum variance method) and physical parameters (fitted with a least-square method) for the small MC. L, G, and H refer to Lundquist, Gold and Hoyle, and Hidalgo et al. model, respectively. The geometrical parameters are: the angle $\theta$ between the axis of the tube and the ecliptic plane, the angle $\varphi$ between the projection of the axis on the ecliptic plane and the abscissa of GSE (anti-clockwise as seen from the positive $z_{\rm GSE}$ axis), and the flux tube radius (R). The two physical parameters are: the twist per unit length ( $\tau _0$ ) and the intensity of the field (B₀), both at the flux tube centre. In the last three columns, we give the computed magnetic flux in the B_z component (F_z), in the $B_{\phi }$ component per unit length ( $F_{\phi }/L$ ) and the magnetic helicity per unit length ( $H_{\rm cloud}/L$ ).
Model $\theta$ $\varphi$ R $\tau _0$ B₀ F_z $F_{\phi }/L$ $H_{\rm cloud}/L$

$^\circ$ $^\circ$ 10^-2 AU AU^-1 nT 10¹⁹ Mx 10¹⁹ Mx/AU 10³⁹ Mx²/AU

L 59 172 1.6 -66 13.8 1.3 20. -3.0

G 59 172 1.6 -85 14.1 1.4 19. -2.8

H 59 172 1.6 -51 15.9 0.9 23. -3.0

**Table 2:** Geometrical (obtained from the minimum variance method) and physical parameters (fitted with a least-square method) for the small MC. L, G, and H refer to Lundquist, Gold and Hoyle, and Hidalgo et al. model, respectively. The geometrical parameters are: the angle $\theta$ between the axis of the tube and the ecliptic plane, the angle $\varphi$ between the projection of the axis on the ecliptic plane and the abscissa of GSE (anti-clockwise as seen from the positive $z_{\rm GSE}$ axis), and the flux tube radius (R). The two physical parameters are: the twist per unit length ( $\tau _0$ ) and the intensity of the field (B₀), both at the flux tube centre. In the last three columns, we give the computed magnetic flux in the B_z component (F_z), in the $B_{\phi }$ component per unit length ( $F_{\phi }/L$ ) and the magnetic helicity per unit length ( $H_{\rm cloud}/L$ ).
Model	$\theta$	$\varphi$	R	$\tau _0$	B₀	F_z	$F_{\phi }/L$	$H_{\rm cloud}/L$
	$^\circ$	$^\circ$	10^-2 AU	AU^-1	nT	10¹⁹ Mx	10¹⁹ Mx/AU	10³⁹ Mx²/AU
L	59	172	1.6	-66	13.8	1.3	20.	-3.0
G	59	172	1.6	-85	14.1	1.4	19.	-2.8
H	59	172	1.6	-51	15.9	0.9	23.	-3.0

Source LaTeX | All tables | In the text

	1 Introduction
	2 Evolution of the small AR during its full life-time
	3 Physical interpretation of the coronal eruptions
	4 Observational evidence of the interplanetary flux rope
	5 Linking the coronal eruption to the interplanetary MC
	6 Conclusions
	References