Resistive evolution of toroidal field distributions and their relation to magnetic clouds

Smiet, C. B.; de Blank, H. J.; de Jong, T. A.; Kok, D. N. L.; Bouwmeester, D.

doi:10.1017/s0022377818001290

Title: Resistive evolution of toroidal field distributions and their relation to magnetic clouds

Journal Article · 21 January 2019 · Journal of Plasma Physics

DOI: https://doi.org/10.1017/s0022377818001290 · OSTI ID:1558790

^[1]; de Blank, H. J. ^[2];

^[3]; Kok, D. N. L. ^[3]; Bouwmeester, D. ^[4]

Princeton Univ., Princeton, NJ (United States). Princeton Plasma Physics Lab; Leiden Univ., Leiden (The Netherlands). Huygens-Kamerlingh Onnes Lab
DIFFER – Dutch Institute for Fundamental Energy Research, Eindhoven (The Netherlands)
Leiden Univ., Leiden (The Netherlands). Huygens-Kamerlingh Onnes Lab
Leiden Univ., Leiden (The Netherlands). Huygens-Kamerlingh Onnes Lab; Univ. of California, Santa Barbara, CA (United States). Dept. of Physics

We study the resistive evolution of a localized self-organizing magnetohydrodynamic equilibrium. In this configuration the magnetic forces are balanced by a pressure force caused by a toroidal depression in the pressure. Equilibrium is attained when this low-pressure region prevents further expansion into the higher-pressure external plasma. We find that, for the parameters investigated, the resistive evolution of the structures follows a universal pattern when rescaled to resistive time. The finite resistivity causes both a decrease in the magnetic field strength and a finite slip of the plasma fluid against the static equilibrium. This slip is caused by a Pfirsch–Schlüter-type diffusion, similar to what is seen in tokamak equilibria. The net effect is that the configuration remains in magnetostatic equilibrium whilst it slowly grows in size. The rotational transform of the structure becomes nearly constant throughout the entire structure, and decreases according to a power law. In simulations this equilibrium is observed when highly tangled field lines relax in a high-pressure (relative to the magnetic field strength) environment, a situation that occurs when the twisted field of a coronal loop is ejected into the interplanetary solar wind. In this study we relate this localized magnetohydrodynamic equilibrium to magnetic clouds in the solar wind.

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Research Organization:: Princeton Plasma Physics Laboratory (PPPL), Princeton, NJ (United States)

Sponsoring Organization:: USDOE

Grant/Contract Number:: AC02-09CH11466

OSTI ID:: 1558790

Journal Information:: Journal of Plasma Physics, Journal Name: Journal of Plasma Physics Journal Issue: 1 Vol. 85; ISSN 0022-3778

Publisher:: Cambridge University PressCopyright Statement

Country of Publication:: United States

Language:: English

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