Expansion of magnetic clouds in the outer heliosphere

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Table 1

Exponents e in the fit with a power law D^e for S, ⟨B⟩, and ⟨N_p⟩ (found by performing a linear fit in log-log plots, Fig. 4).

Range of D^a	S^b	⟨B⟩^b	⟨N_p⟩^b	Ref.^c

all MCs
[1.4,5.4]	0.49±0.26	− 1.20±0.20	− 1.70±0.34	1

non-perturbed and
perturbed MCs
[0.3,1]	0.78±0.12	− 1.85±0.07		2
[1.4,5.4]	0.56±0.34	− 1.18±0.27	− 1.70±0.43	1

non-perturbed MCs
[0.3,1]	0.89±0.15	− 1.85±0.11		2
[1.4,5.4]	0.79±0.46	− 1.39±0.92	− 2.24±0.66	1

perturbed MCs
[0.3,1]	0.45±0.16	− 1.89±0.10		2
[1.4,5.4]	0.54±0.48	− 1.14±0.26	− 1.40±0.50	1

MCs
[0.3,1]			− 2.40±0.30	3
[0.3,1]	1.14±0.44	− 1.64±0.40	− 2.44±0.46	4
[0.3,4.]	0.97±0.10	− 1.80	− 2.8	5
[0.3,4.8]	0.78±0.10			3
[0.3,5.4]	0.61±0.09	− 1.30±0.09	− 2.62±0.07	4
[1.4,5.4]		− 0.88±0.22		4

ICMEs
[0.3,5.4]	0.61	− 1.52		6
[0.3,5.4]	0.92±0.07	− 1.40±0.08	− 2.32±0.07	7

Notes.

^(a)

The range of solar distances is in astronomical units (AU). In the middle part of the table, MCs are separated in non-perturbed and perturbed MCs.

^(b)

The exponents, e, are given for the size S in the direction, the mean magnetic field strength ⟨B⟩, and the mean proton density ⟨N_p⟩. All quantities are computed within the flux rope boundaries.

^(c)

We compare our results with our previous results in the inner heliosphere and with other studies of MCs and ICMEs. The results are from: 1) present work; 2) Gulisano et al. (2010); 3) Bothmer & Schwenn (1998); 4) Leitner et al. (2007); 5) Kumar & Rust (1996); 6) Wang et al. (2005b); 7) Liu et al. (2005).

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