Numerical Simulations of Emerging Magnetic Flux in the Solar Atmosphere: Effects of Partial Ionisation

Details Numerical Simulations of Emerging Magnetic Flux in the Solar Atmosphere: Effects of Partial Ionisation Numerical Simulations of Emerging Magnetic Flux in the Solar Atmosphere: Effects of Partial Ionisation

Jun 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006spd....37.0127l&link_type=abstract

American Astronomical Society, SPD meeting #37, #1.27; Bulletin of the American Astronomical Society, Vol. 38, p.220

Astronomy and Astrophysics

Astronomy

Scientific paper

It has long been accepted that the origins of magnetic field in the solar atmosphere lie in the interior of the Sun. Large scale magnetic field builds up at the base of the convection zone. This field can fragment and form twisted magnetic flux tubes which rise to the surface of the Sun, forming active regions. Less understood is the emergence of field through the stably stratified layers of the solar atmosphere into the corona. One question is how sub-surface magnetic field can become force-free as it emerges into the corona.The lower atmosphere is at sufficiently low temperatures that the fully ionised approximation of MHD is not applicable. The presence of neutrals affects the evolution of the magnetic field in the partially ionised regions of the atmosphere. We present results of large scale numerical simulations of emerging magnetic field in a partially ionised atmosphere. The presence of neutrals leads to a large dissipative region of low magnetic Reynolds number, so that the evolution of the field is diffusion dominated. This region increases rates of the emergence of magnetic flux into the corona. More importantly this dissipative region preferentially dissipates currents perpendicular to the field, and thus provides a mechanism for the formation of force-free coronal magnetic field.

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