The Spreading of X-lines in Three Dimensions during Magnetic Reconnection with a Guide Field

Details The Spreading of X-lines in Three Dimensions during Magnetic Reconnection with a Guide Field The Spreading of X-lines in Three Dimensions during Magnetic Reconnection with a Guide Field

Dec 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011agufmsh13b1939s&link_type=abstract

American Geophysical Union, Fall Meeting 2011, abstract #SH13B-1939

Astronomy and Astrophysics

Astrophysics

[7509] Solar Physics, Astrophysics, And Astronomy / Corona, [7513] Solar Physics, Astrophysics, And Astronomy / Coronal Mass Ejections, [7519] Solar Physics, Astrophysics, And Astronomy / Flares, [7526] Solar Physics, Astrophysics, And Astronomy / Magnetic Reconnection

Scientific paper

Naturally occurring magnetic reconnection often begins in a spatially localized region and spreads in the out-of-plane direction as time progresses. This has been studied by a number of authors for magnetotail applications such as substorms and bursty bulk flows, for which the out-of-plane (guide) field is typically small. However, this same behavior has been observed in laboratory experiments, in two-ribbon solar flares (such as the Bastille Day flare), and at the dayside of the magnetopause. In each of these settings, a significant guide field is present. Without a guide field, it was shown that the reconnection spreading is controlled by the species that carries the current. However, laboratory experiments with a large guide field (Katz et al., Phys. Rev. Lett., 104, 255004, 2010) revealed that the spreading takes place in both directions at the Alfven speed based on the guide magnetic field. We present three-dimensional two-fluid numerical simulations to address the condition on the guide field at which the nature of the spreading switches from being caused by the current carriers to being caused by Alfven waves. Applications for the corona will be discussed.

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