scholarly journals Magnetic Reconnection Inside a Flux Rope Induced by Kelvin‐Helmholtz Vortices

2020 ◽  
Vol 125 (4) ◽  
Author(s):  
K.‐J. Hwang ◽  
K. Dokgo ◽  
E. Choi ◽  
J. L. Burch ◽  
D. G. Sibeck ◽  
...  
Keyword(s):  
Magnetic Reconnection ◽  
Flux Rope

Flux Rope Acceleration and Enhanced Magnetic Reconnection Rate

2003 ◽  
Author(s):  
C.Z. Cheng ◽  
Y. Ren ◽  
G.S. Choe ◽  
Y.-J. Moon
Keyword(s):  
Magnetic Reconnection ◽  
Flux Rope ◽  
Reconnection Rate

scholarly journals Formation of coronal rain triggered by impulsive heating associated with magnetic reconnection

2019 ◽  
Vol 630 ◽  
pp. A123 ◽  
Author(s):  
P. Kohutova ◽  
E. Verwichte ◽  
C. Froment
Keyword(s):  
Magnetic Reconnection ◽  
Thermal Instability ◽  
Flux Rope ◽  
Coronal Loops ◽  
Rain Event ◽  
Subsequent Formation ◽  
Standard Models ◽  
Field Lines ◽  
Impulsive Heating ◽  
Coronal Rain

Context. Coronal rain consists of cool plasma condensations formed in coronal loops as a result of thermal instability. The standard models of coronal rain formation assume that the heating is quasi-steady and localised at the coronal loop footpoints. Aims. We present an observation of magnetic reconnection in the corona and the associated impulsive heating triggering formation of coronal rain condensations. Methods. We analyse combined SDO/AIA and IRIS observations of a coronal rain event following a reconnection between threads of a low-lying prominence flux rope and surrounding coronal field lines. Results. The reconnection of the twisted flux rope and open field lines leads to a release of magnetic twist. Evolution of the emission of one of the coronal loops involved in the reconnection process in different AIA bandpasses suggests that the loop becomes thermally unstable and is subject to the formation of coronal rain condensations following the reconnection and that the associated heating is localised in the upper part of the loop leg. Conclusions. In addition to the standard models of thermally unstable coronal loops with heating localised exclusively in the footpoints, thermal instability and subsequent formation of condensations can be triggered by the impulsive heating associated with magnetic reconnection occurring anywhere along a magnetic field line.

scholarly journals MMS Observation of Secondary Magnetic Reconnection Beside Ion‐Scale Flux Rope at the Magnetopause

2020 ◽  
Vol 47 (16) ◽  
Author(s):  
X.‐C. Dong ◽  
M. W. Dunlop ◽  
T.‐Y. Wang ◽  
K. J. Trattner ◽  
C. T. Russell ◽  
...  
Keyword(s):  
Magnetic Reconnection ◽  
Flux Rope

scholarly journals Solar activities observed with the New Vacuum Solar Telescope

2015 ◽  
Vol 11 (S320) ◽  
pp. 315-320
Author(s):  
Shuhong Yang ◽  
Jun Zhang
Keyword(s):  
Magnetic Reconnection ◽  
Flux Rope ◽  
Observational Evidence ◽  
Small Scale ◽  
Solar Telescope ◽  
New Name ◽  
Direct Observations ◽  
Filament Activation ◽  
First Time

AbstractBased on the New Vacuum Solar Telescope observations, some new results about the solar activities are obtained. (1) In the Hα line, a flux rope tracked by filament activation is detected for the first time. There may exist some mild heating during the filament activation. (2) The direct observations illustrate the mechanism of confined flares, i.e., the flares are triggered by magnetic reconnection between the emerging loops and the pre-existing loops and prevented from being eruptive by the overlying loops. (3) The solid observational evidence of magnetic reconnection between two sets of small-scale loops is reported. The successive slow reconnection changes the conditions around the reconnection area and leads to the rapid reconnection. (4) An ensemble of oscillating bright features rooted in a light bridge is observed and given a new name, light wall. The light wall oscillations may be due to the leakage of p-modes from below the photosphere.

Magnetic Reconnection Rate and Flux‐Rope Acceleration of Two‐Ribbon Flares

2005 ◽  
Vol 620 (2) ◽  
pp. 1085-1091 ◽  
Author(s):  
Ju Jing ◽  
Jiong Qiu ◽  
Jun Lin ◽  
Ming Qu ◽  
Yan Xu ◽  
...  
Keyword(s):  
Magnetic Reconnection ◽  
Flux Rope ◽  
Reconnection Rate

scholarly journals Pulsating Magnetic Reconnection Driven by Three-Dimensional Flux-Rope Interactions

2016 ◽  
Vol 116 (23) ◽  
Author(s):  
W. Gekelman ◽  
T. De Haas ◽  
W. Daughton ◽  
B. Van Compernolle ◽  
T. Intrator ◽  
...  
Keyword(s):  
Magnetic Reconnection ◽  
Three Dimensional ◽  
Flux Rope

scholarly journals Heavy ion escape from Martian wake enhanced by magnetic reconnection

2021 ◽  
Author(s):  
Lei Wang ◽  
Can Huang ◽  
Yasong Ge ◽  
A. M. Du ◽  
Rongsheng Wang ◽  
...  
Keyword(s):  
Magnetic Reconnection ◽  
Flux Rope ◽  
Heavy Ion ◽  
Escape Rate ◽  
Wake Region ◽  
Atmospheric Evolution ◽  
Oxygen Ions ◽  
Plasma Environment ◽  
Ion Escape ◽  
Reconnection Region

Abstract How ion escape from the near-Mars space is one of the biggest puzzles for understanding the atmospheric evolution of Mars. Ions in the plasma wake region continuously escape from the unmagnetized planet. Although the average ion escape rate in the wake region is relatively low, observations also have revealed the presence of events that contribute bursty and enhanced ion escape fluxes. Boundary instabilities and magnetic reconnection are suggested to be the candidate mechanisms. However, there is a lack of evaluation of ion escape caused by reconnection and comparison of the two mechanisms under a similar plasma environment. Here, we show an exciting reconnection event in the Martian wake. Two types of flux ropes are observed during the event. One was generated by reconnection, while others were produced by dayside boundary instability and convected to tail. The escape rate of oxygen ions in the reconnection region was estimated to be about 53–72% of the total tailward escape. Furthermore, the escape flux in the flux rope produced by reconnection was over twice that caused by dayside instabilities.

scholarly journals Simultaneous Observation of a Flux Rope Eruption and Magnetic Reconnection during an X-class Solar Flare

2018 ◽  
Vol 853 (1) ◽  
pp. L18 ◽  
Author(s):  
X. L. Yan ◽  
L. H. Yang ◽  
Z. K. Xue ◽  
Z. X. Mei ◽  
D. F. Kong ◽  
...  
Keyword(s):  
Solar Flare ◽  
Magnetic Reconnection ◽  
Flux Rope ◽  
Simultaneous Observation

scholarly journals A new trigger mechanism for coronal mass ejections

2020 ◽  
Vol 644 ◽  
pp. A137
Author(s):  
A. W. James ◽  
L. M. Green ◽  
L. van Driel-Gesztelyi ◽  
G. Valori
Keyword(s):  
Magnetic Flux ◽  
Magnetic Reconnection ◽  
Extreme Ultraviolet ◽  
Flux Rope ◽  
Active Regions ◽  
Magnetic Activity ◽  
Trigger Mechanism ◽  
Magnetic Flux Rope ◽  
Left Handed ◽  
Flux Ropes

Context. Many previous studies have shown that the magnetic precursor of a coronal mass ejection (CME) takes the form of a magnetic flux rope, and a subset of them have become known as “hot flux ropes” due to their emission signatures in ∼10 MK plasma. Aims. We seek to identify the processes by which these hot flux ropes form, with a view of developing our understanding of CMEs and thereby improving space weather forecasts. Methods. Extreme-ultraviolet observations were used to identify five pre-eruptive hot flux ropes in the solar corona and study how they evolved. Confined flares were observed in the hours and days before each flux rope erupted, and these were used as indicators of episodic bursts of magnetic reconnection by which each flux rope formed. The evolution of the photospheric magnetic field was observed during each formation period to identify the process(es) that enabled magnetic reconnection to occur in the β <  1 corona and form the flux ropes. Results. The confined flares were found to be homologous events and suggest flux rope formation times that range from 18 hours to 5 days. Throughout these periods, fragments of photospheric magnetic flux were observed to orbit around each other in sunspots where the flux ropes had a footpoint. Active regions with right-handed (left-handed) twisted magnetic flux exhibited clockwise (anticlockwise) orbiting motions, and right-handed (left-handed) flux ropes formed. Conclusions. We infer that the orbital motions of photospheric magnetic flux fragments about each other bring magnetic flux tubes together in the corona, enabling component reconnection that forms a magnetic flux rope above a flaring arcade. This represents a novel trigger mechanism for solar eruptions and should be considered when predicting solar magnetic activity.

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