Magnetic Transport on the Solar Atmosphere by Laminar and Turbulent Ambipolar Diffusion

Details Magnetic Transport on the Solar Atmosphere by Laminar and Turbulent Ambipolar Diffusion Magnetic Transport on the Solar Atmosphere by Laminar and Turbulent Ambipolar Diffusion

Sep 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010apj...720.1311h&link_type=abstract

The Astrophysical Journal, Volume 720, Issue 2, pp. 1311-1317 (2010).

Astronomy and Astrophysics

Astronomy

1

Magnetohydrodynamics: Mhd, Sun: Chromosphere, Sun: Dynamo

Scientific paper

The lower solar atmosphere consists of partially ionized turbulent plasmas harboring velocity field, magnetic field, and current density fluctuations. The correlations among these small-scale fluctuations give rise to large-scale flows and magnetic fields which decisively affect all transport processes. The three-fluid system consisting of electrons, ions, and neutral particles supports nonideal effects such as the Hall effect and ambipolar diffusion. Here, we study magnetic transport by the laminar- and turbulent-scale ambipolar diffusion processes using a simple model of the magnetic induction equation. Based on a linear analysis of the induction equation, we perform a one-dimensional numerical simulation to study the laminar ambipolar effect on medium-scale magnetic field structures. The nonlinearity of the laminar ambipolar diffusion creates magnetic structures with sharp gradients in the scale of hundreds of kilometers. We expect that these can be amenable to processes such as magnetic reconnection and energy release therefrom for heating and flaring of the solar plasma. Analyzing the characteristic timescales of these processes, we find that the turbulent diffusion timescale is smaller by several orders of magnitude than the laminar diffusion timescale. The effect of the modeled turbulent ambipolar diffusion on the obtained field structures is briefly discussed.

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