Solar coronal heating by magnetic cancellation

B. Von Rekowski; C. E. Parnell; E. R. Priest

Solar coronal heating by magnetic cancellation

B. Von Rekowski^*, C. E. Parnell, E. R. Priest

^*Corresponding author for this work

Research output: Contribution to specialist publication › Article

Abstract

We present two-dimensional numerical magnetohydro-dynamic simulations of a cancelling magnetic feature and the associated coronal X-ray bright point. Coronal reconnection is found to produce significant Ohmic heating, and at the same time at least 90 to 95% of the magnetic flux of the converging bipole is cancelled. The last at most 5 to 10% is cancelled when reconnection occurs at the base. Reconnection happens in a time-dependent way in response to the driven footpoint motions.

Original language	English
Pages	193-196
Number of pages	4
No.	600
Specialist publication	European Space Agency, (Special Publication) ESA SP
Publication status	Published - 1 Dec 2005

Keywords

Cancellation
Coronal heating
Magnetic fields
Magnetohydrodynamics (MHD)
Reconnection

Cite this

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title = "Solar coronal heating by magnetic cancellation",

abstract = "We present two-dimensional numerical magnetohydro-dynamic simulations of a cancelling magnetic feature and the associated coronal X-ray bright point. Coronal reconnection is found to produce significant Ohmic heating, and at the same time at least 90 to 95% of the magnetic flux of the converging bipole is cancelled. The last at most 5 to 10% is cancelled when reconnection occurs at the base. Reconnection happens in a time-dependent way in response to the driven footpoint motions.",

keywords = "Cancellation, Coronal heating, Magnetic fields, Magnetohydrodynamics (MHD), Reconnection",

author = "{Von Rekowski}, B. and Parnell, {C. E.} and Priest, {E. R.}",

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AU - Von Rekowski, B.

AU - Parnell, C. E.

AU - Priest, E. R.

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N2 - We present two-dimensional numerical magnetohydro-dynamic simulations of a cancelling magnetic feature and the associated coronal X-ray bright point. Coronal reconnection is found to produce significant Ohmic heating, and at the same time at least 90 to 95% of the magnetic flux of the converging bipole is cancelled. The last at most 5 to 10% is cancelled when reconnection occurs at the base. Reconnection happens in a time-dependent way in response to the driven footpoint motions.

AB - We present two-dimensional numerical magnetohydro-dynamic simulations of a cancelling magnetic feature and the associated coronal X-ray bright point. Coronal reconnection is found to produce significant Ohmic heating, and at the same time at least 90 to 95% of the magnetic flux of the converging bipole is cancelled. The last at most 5 to 10% is cancelled when reconnection occurs at the base. Reconnection happens in a time-dependent way in response to the driven footpoint motions.

KW - Cancellation

KW - Coronal heating

KW - Magnetic fields

KW - Magnetohydrodynamics (MHD)

KW - Reconnection

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M3 - Article

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JO - European Space Agency, (Special Publication) ESA SP

JF - European Space Agency, (Special Publication) ESA SP

ER -

Solar coronal heating by magnetic cancellation

Abstract

Keywords

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