scholarly journals Magnetohydrodynamic Simulation of Solar Coronal Chromospheric Evaporation Jets Caused by Magnetic Reconnection Associated with Magnetic Flux Emergence

2004 ◽  
Vol 614 (2) ◽  
pp. 1042-1053 ◽  
Author(s):  
Takehiro Miyagoshi ◽  
Takaaki Yokoyama
Keyword(s):  
Magnetic Flux ◽  
Magnetic Reconnection ◽  
Flux Emergence ◽  
Chromospheric Evaporation ◽  
Magnetohydrodynamic Simulation ◽  
Solar Coronal

scholarly journals Multiple Solar Jets from NOAA AR 12644

2018 ◽  
Vol 13 (S340) ◽  
pp. 177-178 ◽  
Author(s):  
Reetika Joshi ◽  
Ramesh Chandra
Keyword(s):  
Active Region ◽  
Magnetic Flux ◽  
Magnetic Reconnection ◽  
Spatial Resolution ◽  
Null Point ◽  
Flux Emergence ◽  
Temporal And Spatial ◽  
Noaa Active Region ◽  
Multi Band

AbstractWe present here the observations of solar jets observed on April 04, 2017 from NOAA active region (AR) 12644 using high temporal and spatial resolution AIA instrument. We have observed around twelve recurring jets during the whole day. Magnetic flux emergence and cancellation have been observed at the jet location. The multi-band observations evidenced that these jets were triggered due to the magnetic reconnection at low coronal null–point.

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.

scholarly journals Simulations of Switchback, Fragmentation and Sunspot Pair in δ-Sunspots during Magnetic Flux Emergence

Sensors ◽  
2021 ◽  
Vol 21 (2) ◽  
pp. 586
Author(s):  
Che-Jui Chang ◽  
Jean-Fu Kiang
Keyword(s):  
Magnetic Field ◽  
Solar System ◽  
Field Strength ◽  
Magnetic Flux ◽  
Initial Conditions ◽  
Observation Data ◽  
Flux Emergence ◽  
Polarity Inversion ◽  
Simulation Results ◽  
Spot Type

Strong flares and coronal mass ejections (CMEs), launched from δ-sunspots, are the most catastrophic energy-releasing events in the solar system. The formations of δ-sunspots and relevant polarity inversion lines (PILs) are crucial for the understanding of flare eruptions and CMEs. In this work, the kink-stable, spot-spot-type δ-sunspots induced by flux emergence are simulated, under different subphotospheric initial conditions of magnetic field strength, radius, twist, and depth. The time evolution of various plasma variables of the δ-sunspots are simulated and compared with the observation data, including magnetic bipolar structures, relevant PILs, and temperature. The simulation results show that magnetic polarities display switchbacks at a certain stage and then split into numerous fragments. The simulated fragmentation phenomenon in some δ-sunspots may provide leads for future observations in the field.

scholarly journals Magnetic Flux Emergence and Decay Rates for Preceder and Follower Sunspots Observed with HMI

2017 ◽  
Vol 842 (1) ◽  
pp. 3 ◽  
Author(s):  
A. A. Norton ◽  
E. H. Jones ◽  
M. G. Linton ◽  
J. E. Leake
Keyword(s):  
Magnetic Flux ◽  
Decay Rates ◽  
Flux Emergence

scholarly journals Magnetic reconnection resulting from flux emergence: implications for jet formation in the lower solar atmosphere?

2011 ◽  
Vol 535 ◽  
pp. A95 ◽  
Author(s):  
J. Y. Ding ◽  
M. S. Madjarska ◽  
J. G. Doyle ◽  
Q. M. Lu ◽  
K. Vanninathan ◽  
...  
Keyword(s):  
Magnetic Reconnection ◽  
Solar Atmosphere ◽  
Flux Emergence ◽  
Jet Formation ◽  
Lower Solar Atmosphere
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