Solar coronal heating by magnetic cancellation - II. Disconnected and unequal bipoles

Details Solar coronal heating by magnetic cancellation - II. Disconnected and unequal bipoles Solar coronal heating by magnetic cancellation - II. Disconnected and unequal bipoles

Jun 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006mnras.369...43v&link_type=abstract

Monthly Notices of the Royal Astronomical Society, Volume 369, Issue 1, pp. 43-56.

Astronomy and Astrophysics

Astronomy

10

Mhd: Sun: Corona: Sun: Magnetic Fields, Mhd, Sun: Corona, Sun: Magnetic Fields

Scientific paper

Two-dimensional numerical magnetohydrodynamic simulations of a cancelling magnetic feature (CMF) and the associated coronal X-ray bright point (XBP) are presented. Coronal magnetic reconnection is found to produce the Ohmic heating required for a coronal XBP. During the BP phase where reconnection occurs above the base, about 90-95 per cent of the magnetic flux of the converging magnetic bipole cancels at the base. The last ~5 to 10 per cent of the base magnetic flux is cancelled when reconnection occurs at the base. Reconnection happens in a time-dependent way in response to the imposed converging footpoint motions. A potential field model gives a good first approximation to the qualitative behaviour of the system, but the magnetohydrodynamics (MHD) experiments reveal several quantitative differences: for example, the effects of plasma inertia and a pressure build-up in-between the converging bipole are to delay the onset of coronal reconnection above the base and to lower the maximum X-point height.

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