scholarly journals Acceleration of the Solar Wind as a Result of the Reconnection of Open Magnetic Flux with Coronal Loops

2003 ◽  
Author(s):  
L. A. Fisk
Keyword(s):  
Solar Wind ◽  
Magnetic Flux ◽  
Coronal Loops ◽  
Open Magnetic Flux

scholarly journals Solar wind elemental abundances related to the Sun's open magnetic flux

2009 ◽  
Vol 505 (3) ◽  
pp. 1237-1244 ◽  
Author(s):  
X. Wang ◽  
B. Klecker ◽  
P. Wurz
Keyword(s):  
Solar Wind ◽  
Magnetic Flux ◽  
Elemental Abundances ◽  
Open Magnetic Flux

scholarly journals Energetics of magnetic transients in a solar active region plage

2019 ◽  
Vol 623 ◽  
pp. A176 ◽  
Author(s):  
L. P. Chitta ◽  
A. R. C. Sukarmadji ◽  
L. Rouppe van der Voort ◽  
H. Peter
Keyword(s):  
Magnetic Field ◽  
Active Region ◽  
Magnetic Flux ◽  
Numerical Simulations ◽  
Extreme Ultraviolet ◽  
Spatial Scales ◽  
Coronal Loops ◽  
The Sun ◽  
Flux Emergence ◽  
Transient Events

Context. Densely packed coronal loops are rooted in photospheric plages in the vicinity of active regions on the Sun. The photospheric magnetic features underlying these plage areas are patches of mostly unidirectional magnetic field extending several arcsec on the solar surface. Aims. We aim to explore the transient nature of the magnetic field, its mixed-polarity characteristics, and the associated energetics in the active region plage using high spatial resolution observations and numerical simulations. Methods. We used photospheric Fe I 6173 Å spectropolarimetric observations of a decaying active region obtained from the Swedish 1-m Solar Telescope (SST). These data were inverted to retrieve the photospheric magnetic field underlying the plage as identified in the extreme-ultraviolet emission maps obtained from the Atmospheric Imaging Assembly (AIA) on board the Solar Dynamics Observatory (SDO). To obtain better insight into the evolution of extended unidirectional magnetic field patches on the Sun, we performed 3D radiation magnetohydrodynamic simulations of magnetoconvection using the MURaM code. Results. The observations show transient magnetic flux emergence and cancellation events within the extended predominantly unipolar patch on timescales of a few 100 s and on spatial scales comparable to granules. These transient events occur at the footpoints of active region plage loops. In one case the coronal response at the footpoints of these loops is clearly associated with the underlying transient. The numerical simulations also reveal similar magnetic flux emergence and cancellation events that extend to even smaller spatial and temporal scales. Individual simulated transient events transfer an energy flux in excess of 1 MW m−2 through the photosphere. Conclusions. We suggest that the magnetic transients could play an important role in the energetics of active region plage. Both in observations and simulations, the opposite-polarity magnetic field brought up by transient flux emergence cancels with the surrounding plage field. Magnetic reconnection associated with such transient events likely conduits magnetic energy to power the overlying chromosphere and coronal loops.

FeNi-based flat magnetoimpedance nanostructures with open magnetic flux: New topological approaches

2015 ◽  
Vol 383 ◽  
pp. 220-225 ◽  
Author(s):  
G.V. Kurlyandskaya ◽  
A.A. Chlenova ◽  
E. Fernández ◽  
K.J. Lodewijk
Keyword(s):  
Magnetic Flux ◽  
Open Magnetic Flux

scholarly journals Dayside auroral activity and magnetic flux transfer from the solar wind

1989 ◽  
Vol 16 (1) ◽  
pp. 33-36 ◽  
Author(s):  
M. Lockwood ◽  
P. E. Sandholt ◽  
S. W. H. Cowley
Keyword(s):  
Solar Wind ◽  
Magnetic Flux ◽  
Auroral Activity ◽  
Flux Transfer

scholarly journals Aurora and open magnetic flux during isolated substorms, sawteeth, and SMC events

2007 ◽  
Vol 25 (8) ◽  
pp. 1865-1876 ◽  
Author(s):  
A. D. DeJong ◽  
X. Cai ◽  
R. C. Clauer ◽  
J. F. Spann
Keyword(s):  
Magnetic Flux ◽  
Temporal Variations ◽  
Auroral Oval ◽  
Polar Cap ◽  
Expansion Phase ◽  
Magnetospheric Convection ◽  
Open Magnetic Flux ◽  
Open Flux ◽  
The Individual

Abstract. Using Polar UVI LBHl and IMAGE FUV WIC data, we have compared the auroral signatures and polar cap open flux for isolated substorms, sawteeth oscillations, and steady magnetospheric convection (SMC) events. First, a case study of each event type is performed, comparing auroral signatures and open magnetic fluxes to one another. The latitude location of the auroral oval is similar during isolated substorms and SMC events. The auroral intensity during SMC events is similar to that observed during the expansion phase of an isolated substorm. Examination of an individual sawtooth shows that the auroral intensity is much greater than the SMC or isolated substorm events and the auroral oval is displaced equatorward making a larger polar cap. The temporal variations observed during the individual sawtooth are similar to that observed during the isolated substorm, and while the change in polar cap flux measured during the sawtooth is larger, the percent change in flux is similar to that measured during the isolated substorm. These results are confirmed by a statistical analysis of events within these three classes. The results show that the auroral oval measured during individual sawteeth contains a polar cap with, on average, 150% more magnetic flux than the oval measured during isolated substorms or during SMC events. However, both isolated substorms and sawteeth show a 30% decrease in polar cap magnetic flux during the dipolarization (expansion) phase.

scholarly journals Generation of Inverted Heliospheric Magnetic Flux by Coronal Loop Opening and Slow Solar Wind Release

2018 ◽  
Vol 868 (1) ◽  
pp. L14 ◽  
Author(s):  
Mathew J. Owens ◽  
Mike Lockwood ◽  
Luke A. Barnard ◽  
Allan R. MacNeil
Keyword(s):  
Solar Wind ◽  
Magnetic Flux ◽  
Coronal Loop ◽  
Slow Solar Wind
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