Three-dimensional Resistive-MHD Model for X-ray Bright Points and Coronal Jets

Details Three-dimensional Resistive-MHD Model for X-ray Bright Points and Coronal Jets Three-dimensional Resistive-MHD Model for X-ray Bright Points and Coronal Jets

Dec 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007agufmsh21b..03p&link_type=abstract

American Geophysical Union, Fall Meeting 2007, abstract #SH21B-03

Physics

7509 Corona, 7524 Magnetic Fields, 7526 Magnetic Reconnection (2723, 7835)

Scientific paper

Thirteen years ago a simple two-dimensional model for an X-ray bright point and associated cancelling magnetic feature was first proposed by Priest et. al (1994). Over the next decade this model was extended into three- dimensions and applied by many authors to many observed X-ray bright points. A two-dimensional model was proposed at about the same time for coronal jets associated with the emergence of magnetic flux (e.g. Yokoyama & Shibata 1995). Recently, however, new results from Hinode hint to the fact that X-ray bright points may not actually be created cancellation. Furthermore, images from XRT aboard Hinode reveal that coronal jets occur far more frequency than previously reported. We present results from resistive MHD experiments that show how it is possible to create an X-ray bright point and coronal jet without the need for either the emergence or cancellation of magnetic flux. Thus, the numbers of each event are not limited to the numbers of flux emergences or cancellations. Moreover, by following the evolution of the magnetic topology during the interaction we can show that reconnection at multiple (as opposed to single) separators is the energy release mechanism. Also, we reveal how it is possible to get dramatic changes in the coronal loop structures observed with hardly any changes in the magnetic footpoints below, in line with recent observations from Hinode.

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