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Abstract
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 approximate to 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.
Original language | English |
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Pages (from-to) | 43-56 |
Number of pages | 14 |
Journal | Monthly Notices of the Royal Astronomical Society |
Volume | 369 |
DOIs | |
Publication status | Published - 11 Jun 2006 |
Keywords
- MHD
- Sun : corona
- Sun : magnetic fields
- RAY BRIGHT POINTS
- CONVERGING FLUX MODEL
- CURRENT SHEETS
- QUIET SUN
- RECONNECTION
- REGIONS
- DRIVEN
- EVENTS
- SITES
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Dive into the research topics of 'Solar coronal heating by magnetic cancellation: II Disconnected and unequal bipoles'. Together they form a unique fingerprint.Projects
- 1 Finished
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Solar&Magnetospheric Plasma Theory PP/E1: Solar and Magnetospheric Plasma Theory
Neukirch, T. (PI), Hood, A. W. (CoI), Parnell, C. E. (CoI), Priest, E. (CoI), Roberts, B. (CoI) & Wright, A. N. (CoI)
1/04/07 → 31/03/12
Project: Standard