Global and local expansion of magnetic clouds in the inner heliosphere

A. M. Gulisano; P. Démoulin; S. Dasso; M. E. Ruiz; E. Marsch

doi:10.1051/0004-6361/200912375

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Volume 509 (January 2010)

A&A, 509 (2010) A39

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Table 1:

List of MC events.
$\begin{displaymath}{\begin{tabular}{cc@{ }cr@{.}lr@{.}l} \hline\hline S/C & $T... ...N & 10&0 $\pm$ 6.4 & 0&91 $\pm$ 0.23\\ \hline \end{tabular}} \end{displaymath}$ The first column in Table 1 indicates the spacecraft (Helios 1 or Helios 2), $T_{\rm c}$ in the second column is the time for the observation of the MC center (or for the minimum approach distance). The MCs are separated in two groups: perturbed (P) and non-perturbed (N) by a fast SW stream. $\Delta V_x/(t_{\rm out}-t_{\rm in})$ is minus the fitted slope of the temporal velocity profile (see, Eq. (2)) and $\zeta$ is the non-dimensional expansion coefficient (Eq. (8)). $\Delta V_x/(t_{\rm out}-t_{\rm in})<0$ means observed compression of the MC. The average values and the standard deviations are given at the bottom.

Source LaTeX | All tables | In the text

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