Expansion of magnetic clouds in the outer heliosphere

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Table 2

Average and dispersion in the main parameters of MCs from our present study and Du et al. (2010).

Group^a	V_c^b	S_1 AU^c	⟨B⟩_1 AU^c	⟨N_p⟩_1 AU^c	⟨β_p⟩	γ^d	ζ^e
	km s^-1	AU	nT	cm^-3		°

all MCs	470 ± 110	0.16 ± 0.12	12 ± 7	9 ± 8	0.19 ± 0.17	68 ± 17	0.77 ± 0.75
non-perturbed and perturbed	480 ± 120	0.18 ± 0.14	14 ± 8	9 ± 8	0.18 ± 0.19	68 ± 20	0.63 ± 0.59
non-perturbed	480 ± 130	0.24 ± 0.16	11 ± 9	7 ± 10	0.17 ± 0.18	63 ± 24	1.05 ± 0.34
perturbed	480 ± 110	0.13 ± 0.09	16 ± 6	11 ± 7	0.19 ± 0.20	72 ± 15	0.28 ± 0.52
interacting	470 ± 130	0.12 ± 0.05	10 ± 6	9 ± 9	0.22 ± 0.14	66 ± 13	1.00 ± 0.93
MC^f	500 ± 100	0.26 ± 0.19	11 ± 6				0.59 ± 0.51
non-MC ICME^f	480 ± 90	0.22 ± 0.21	5 ± 4				0.68 ± 0.48

Notes.

^(a)

The MCs are separated into three groups: non-perturbed, perturbed, and interacting.

^(b)

V_c is the velocity at the closest distance from the MC center.

^(c)

The size and the mean field are normalized to 1 AU according to Eq. (8) and the proton density with ⟨N_p⟩_1 AU = ⟨N_p⟩D^2.2, where D is the solar distance in AU.

^(d)

γ is the angle between the MC axis and the radial direction ().

^(e)

ζ is the nondimensional expansion rate (Eq. (5)).

^(f)

Computed from the results of Du et al. (2010).

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