Kinematic magnetic reconnection at 3D null points

D. I. Pontin; G. Hornig; E. R. Priest

Kinematic magnetic reconnection at 3D null points

Research output: Chapter in Book/Report/Conference proceeding › Other chapter contribution

Abstract

Magnetic reconnection at a three-dimensional null point is the natural extension of the familiar two-dimensional X-point reconnection. Three dimensional null points are found in abundance in the solar corona, where they are thought to be an important feature with regards to the coronal heating problem. A model is set up here for reconnection at a 3D magnetic null point, by solving the kinematic, steady, resistive MHD equations in its vicinity. A steady magnetic field is assumed, as well as the existence of a localised diffusion region surrounding the null point. Particular attention is focused on the way that the magnetic flux changes its connections as a result of the reconnection process. The nature of the flows and the reconnection is found to be fundamentally different depending on the orientation of the electric current.

Original language	English
Title of host publication	Proceedings of the SOHO 15 Workshop, Coronal Heating, 6-9 September 2004, St Andrews, Scotland
Editors	R. W. Walsh, J. Ireland, D. Danesy, B. Fleck
Publication status	Published - 2004
Event	SOHO 15 Workshop, Coronal Heating - St Andrews, United Kingdom Duration: 6 Sept 2004 → 9 Sept 2004

Workshop

Workshop	SOHO 15 Workshop, Coronal Heating
Country/Territory	United Kingdom
City	St Andrews
Period	6/09/04 → 9/09/04

Keywords

Magnetic reconnection
Magnetohydrodynamics (MHD)
Magnetic null points
MHD

Embargoed Document

Soho15
421 KB
Embargo ends: 31/12/99

Cite this

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title = "Kinematic magnetic reconnection at 3D null points",

abstract = "Magnetic reconnection at a three-dimensional null point is the natural extension of the familiar two-dimensional X-point reconnection. Three dimensional null points are found in abundance in the solar corona, where they are thought to be an important feature with regards to the coronal heating problem. A model is set up here for reconnection at a 3D magnetic null point, by solving the kinematic, steady, resistive MHD equations in its vicinity. A steady magnetic field is assumed, as well as the existence of a localised diffusion region surrounding the null point. Particular attention is focused on the way that the magnetic flux changes its connections as a result of the reconnection process. The nature of the flows and the reconnection is found to be fundamentally different depending on the orientation of the electric current.",

keywords = "Magnetic reconnection, Magnetohydrodynamics (MHD), Magnetic null points, MHD",

author = "Pontin, \{D. I.\} and G. Hornig and Priest, \{E. R.\}",

note = "dc.description.sponsorship: Particle Physics and Astronomy Research Council European Community Human Potential dc.ispartof: ESA;SP-575 ; SOHO 15 Workshop, Coronal Heating ; Conference date: 06-09-2004 Through 09-09-2004",

year = "2004",

language = "English",

isbn = "9290928867",

editor = "Walsh, \{R. W.\} and J. Ireland and D. Danesy and B. Fleck",

booktitle = "Proceedings of the SOHO 15 Workshop, Coronal Heating, 6-9 September 2004, St Andrews, Scotland",

}

TY - CHAP

T1 - Kinematic magnetic reconnection at 3D null points

AU - Pontin, D. I.

AU - Hornig, G.

AU - Priest, E. R.

N1 - dc.description.sponsorship: Particle Physics and Astronomy Research Council European Community Human Potential dc.ispartof: ESA;SP-575

PY - 2004

Y1 - 2004

N2 - Magnetic reconnection at a three-dimensional null point is the natural extension of the familiar two-dimensional X-point reconnection. Three dimensional null points are found in abundance in the solar corona, where they are thought to be an important feature with regards to the coronal heating problem. A model is set up here for reconnection at a 3D magnetic null point, by solving the kinematic, steady, resistive MHD equations in its vicinity. A steady magnetic field is assumed, as well as the existence of a localised diffusion region surrounding the null point. Particular attention is focused on the way that the magnetic flux changes its connections as a result of the reconnection process. The nature of the flows and the reconnection is found to be fundamentally different depending on the orientation of the electric current.

AB - Magnetic reconnection at a three-dimensional null point is the natural extension of the familiar two-dimensional X-point reconnection. Three dimensional null points are found in abundance in the solar corona, where they are thought to be an important feature with regards to the coronal heating problem. A model is set up here for reconnection at a 3D magnetic null point, by solving the kinematic, steady, resistive MHD equations in its vicinity. A steady magnetic field is assumed, as well as the existence of a localised diffusion region surrounding the null point. Particular attention is focused on the way that the magnetic flux changes its connections as a result of the reconnection process. The nature of the flows and the reconnection is found to be fundamentally different depending on the orientation of the electric current.

KW - Magnetic reconnection

KW - Magnetohydrodynamics (MHD)

KW - Magnetic null points

KW - MHD

M3 - Other chapter contribution

SN - 9290928867

BT - Proceedings of the SOHO 15 Workshop, Coronal Heating, 6-9 September 2004, St Andrews, Scotland

A2 - Walsh, R. W.

A2 - Ireland, J.

A2 - Danesy, D.

A2 - Fleck, B.

T2 - SOHO 15 Workshop, Coronal Heating

Y2 - 6 September 2004 through 9 September 2004

ER -

Kinematic magnetic reconnection at 3D null points

Abstract

Workshop

Keywords

Embargoed Document

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