Chromospheric Magnetic Reconnection and its Implication for Coronal Heating

1999 ◽  
Vol 524 (1) ◽  
pp. L75-L78 ◽  
Author(s):  
P. A. Sturrock ◽  
C. B. Roald ◽  
R. Wolfson
Keyword(s):  
Magnetic Reconnection ◽  
Coronal Heating

Solar coronal heating by forced magnetic reconnection: Multiple reconnection events

2005 ◽  
Vol 12 (1) ◽  
pp. 012904 ◽  
Author(s):  
Rekha Jain ◽  
Philippa Browning ◽  
K. Kusano
Keyword(s):  
Magnetic Reconnection ◽  
Coronal Heating ◽  
Forced Magnetic Reconnection ◽  
Solar Coronal

Coronal Heating: Energy Release Associated with Chromospheric Magnetic Reconnection

2000 ◽  
Vol 538 (2) ◽  
pp. 960-967 ◽  
Author(s):  
Colin B. Roald ◽  
P. A. Sturrock ◽  
Richard Wolfson
Keyword(s):  
Magnetic Reconnection ◽  
Energy Release ◽  
Coronal Heating

Coronal heating by magnetic reconnection

1996 ◽  
Vol 237 (1-2) ◽  
pp. 49-73 ◽  
Author(s):  
Eric R. Priest
Keyword(s):  
Magnetic Reconnection ◽  
Coronal Heating

scholarly journals Coronal heating by magnetic reconnection in loops with zero net current

2009 ◽  
Vol 506 (2) ◽  
pp. 913-925 ◽  
Author(s):  
A. W. Hood ◽  
P. K. Browning ◽  
R. A. M. Van der Linden
Keyword(s):  
Magnetic Reconnection ◽  
Coronal Heating

scholarly journals Relating magnetic reconnection to coronal heating

2015 ◽  
Vol 373 (2042) ◽  
pp. 20140263 ◽  
Author(s):  
D. W. Longcope ◽  
L. A. Tarr
Keyword(s):  
Energy Dissipation ◽  
Magnetic Fields ◽  
Solar Corona ◽  
Magnetic Reconnection ◽  
Active Regions ◽  
Coronal Heating ◽  
Flux Emergence ◽  
Coronal Magnetic Fields ◽  
Field Lines ◽  
A Current

It is clear that the solar corona is being heated and that coronal magnetic fields undergo reconnection all the time. Here we attempt to show that these two facts are related—i.e. coronal reconnection generates heat. This attempt must address the fact that topological change of field lines does not automatically generate heat. We present one case of flux emergence where we have measured the rate of coronal magnetic reconnection and the rate of energy dissipation in the corona. The ratio of these two, , is a current comparable to the amount of current expected to flow along the boundary separating the emerged flux from the pre-existing flux overlying it. We can generalize this relation to the overall corona in quiet Sun or in active regions. Doing so yields estimates for the contribution to coronal heating from magnetic reconnection. These estimated rates are comparable to the amount required to maintain the corona at its observed temperature.

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