A note on generalized twisted fields and autotopisms of translation planes

2010 ◽  
Vol 47 (3) ◽  
pp. 311-320
Author(s):  
Mashhour Alali ◽  
Sahem Tarawneh
Keyword(s):  
Translation Planes ◽  
Twisted Field ◽  
Twisted Fields

The first part of this paper is a discussion of autotopism groups of certain translation planes. The second part shows that there is a certain class of semifields of order q4 having nuclei of order q2 , and their translation planes are not desarguesian and not isomorphic to generalized twisted field planes.

Translation planes admitting many homologies

1994 ◽  
Vol 49 (1-2) ◽  
pp. 117-149 ◽  
Author(s):  
Norman L. Johnson ◽  
Rolando Pomareda
Keyword(s):  
Translation Planes

Axisymmetric magnetoconvection in a twisted field

1993 ◽  
Vol 253 (-1) ◽  
pp. 297 ◽  
Author(s):  
C. A. Jones ◽  
D. J. Galloway
Keyword(s):  
Twisted Field

scholarly journals TWISTED FIELD WORKING Fighting for the Relevance of Being Connected

2011 ◽  
Vol 41 (1) ◽  
Author(s):  
Kirsti Mathiesen Hjemdahl Mathiesen Hjemdahl
Keyword(s):  
Twisted Field

scholarly journals On Transposed Translation Planes

2012 ◽  
Vol 02 (01) ◽  
pp. 35-43
Author(s):  
K. Satyanarayana ◽  
K. V. V. N. S. Sundari Kameswari
Keyword(s):  
Translation Planes

scholarly journals Formation of Magnetic Flux Rope During Solar Eruption. I. Evolution of Toroidal Flux and Reconnection Flux

2021 ◽  
Vol 9 ◽  
Author(s):  
Chaowei Jiang ◽  
Jun Chen ◽  
Aiying Duan ◽  
Xinkai Bian ◽  
Xinyi Wang ◽  
...  
Keyword(s):  
Magnetic Flux ◽  
Early Phase ◽  
Flux Rope ◽  
Three Dimensions ◽  
Bottom Surface ◽  
Peak Time ◽  
Magnetic Flux Ropes ◽  
Twisted Field ◽  
Solar Eruptions ◽  
Field Lines

Magnetic flux ropes (MFRs) constitute the core structure of coronal mass ejections (CMEs), but hot debates remain on whether the MFR forms before or during solar eruptions. Furthermore, how flare reconnection shapes the erupting MFR is still elusive in three dimensions. Here we studied a new MHD simulation of CME initiation by tether-cutting magnetic reconnection in a single magnetic arcade. The simulation follows the whole life, including the birth and subsequent evolution, of an MFR during eruption. In the early phase, the MFR is partially separated from its ambient field by a magnetic quasi-separatrix layer (QSL) that has a double-J shaped footprint on the bottom surface. With the ongoing of the reconnection, the arms of the two J-shaped footprints continually separate from each other, and the hooks of the J shaped footprints expand and eventually become closed almost at the eruption peak time, and thereafter the MFR is fully separated from the un-reconnected field by the QSL. We further studied the evolution of the toroidal flux in the MFR and compared it with that of the reconnected flux. Our simulation reproduced an evolution pattern of increase-to-decrease of the toroidal flux, which is reported recently in observations of variations in flare ribbons and transient coronal dimming. The increase of toroidal flux is owing to the flare reconnection in the early phase that transforms the sheared arcade to twisted field lines, while its decrease is a result of reconnection between field lines in the interior of the MFR in the later phase.

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