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Magnetic field line braiding in the solar atmosphere

Published online by Cambridge University Press:  12 September 2017

S. Candelaresi ,
D. I. Pontin  and
G. Hornig
S. Candelaresi
Affiliation:
Division of Mathematics, University of Dundee, Dundee, DD1 4HN, UK
D. I. Pontin
Affiliation:
Division of Mathematics, University of Dundee, Dundee, DD1 4HN, UK
G. Hornig
Affiliation:
Division of Mathematics, University of Dundee, Dundee, DD1 4HN, UK
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Abstract

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Using a magnetic carpet as model for the near surface solar magnetic field we study its effects on the propagation of energy injectected by photospheric footpoint motions. Such a magnetic carpet structure is topologically highly non-trivial and with its magnetic nulls exhibits qualitatively different behavior than simpler magnetic fields. We show that the presence of magnetic fields connecting back to the photosphere inhibits the propagation of energy into higher layers of the solar atmosphere, like the solar corona. By applying certain types of footpoint motions the magnetic field topology is is greatly reduced through magnetic field reconnection which facilitates the propagation of energy and disturbances from the photosphere.

Keywords

Sun: photosphereSun: magnetic fieldsSun: sunspotsmagnetic reconnectionmagnetohydrodynamics (MHD)plasmas
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 12 , Symposium S327: Fine Structure and Dynamics of the Solar Atmosphere , October 2016 , pp. 77 - 81
Copyright
Copyright © International Astronomical Union 2017 

References

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