Interplanetary Magnetic Flux Ropes as Agents Connecting Solar Eruptions and Geomagnetic Activities

Solar Physics ◽  
2017 ◽  
Vol 292 (12) ◽  
Author(s):  
K. Marubashi ◽  
K.-S. Cho ◽  
H. Ishibashi
Keyword(s):  
Magnetic Flux ◽  
Magnetic Flux Ropes ◽  
Flux Ropes ◽  
Solar Eruptions ◽  
Geomagnetic Activities

Evidence for Helically Kinked Magnetic Flux Ropes in Solar Eruptions

1996 ◽  
Vol 464 (2) ◽  
pp. L199-L202 ◽  
Author(s):  
D. M. Rust ◽  
A. Kumar
Keyword(s):  
Magnetic Flux ◽  
Magnetic Flux Ropes ◽  
Flux Ropes ◽  
Solar Eruptions

scholarly journals Observations of Magnetic Flux Ropes Opened or Disconnected From the Sun by Magnetic Reconnection in Interplanetary Space

2021 ◽  
Vol 9 ◽  
Author(s):  
Hengqiang Feng ◽  
Yan Zhao ◽  
Jiemin Wang ◽  
Qiang Liu ◽  
Guoqing Zhao
Keyword(s):  
Magnetic Field ◽  
Magnetic Flux ◽  
Magnetic Reconnection ◽  
Interplanetary Space ◽  
Closed Field ◽  
Magnetic Flux Ropes ◽  
Flux Ropes ◽  
Solar Eruptions ◽  
Wind Spacecraft ◽  
Field Lines

During solar eruptions, many closed magnetic flux ropes are ejected into interplanetary space, which contribute to the heliospheric magnetic field and have important space weather effect because of their coherent magnetic field. Therefore, understanding the evolution of these closed flux ropes in the interplanetary space is important. In this paper, we examined all the magnetic and plasma data measured in 1997 by the Wind spacecraft and identified 621 reconnection exhausts. Of the 621 reconnection events, 31 were observed at the boundaries of magnetic flux ropes and were thought to cause the opening or disconnection magnetic field lines of the adjacent ropes. Of the 31 magnetic reconnection events, 29 were interchange reconnections and the closed field lines of these related flux ropes were opened by them. Only 2 of the 31 magnetic reconnection events disconnected the opened field lines of the original flux ropes. These observations indicate that interchange reconnection and disconnection may be two important mechanisms changing the magnetic topology of the magnetic flux ropes during their propagation during the interplanetary space.

scholarly journals When do solar erupting hot magnetic flux ropes form?

2020 ◽  
Vol 642 ◽  
pp. A109 ◽  
Author(s):  
A. Nindos ◽  
S. Patsourakos ◽  
A. Vourlidas ◽  
X. Cheng ◽  
J. Zhang
Keyword(s):  
Magnetic Flux ◽  
Flux Rope ◽  
Flare Activity ◽  
Solar Dynamics Observatory ◽  
Magnetic Flux Ropes ◽  
Morphological Criteria ◽  
Flux Ropes ◽  
Solar Eruptions ◽  
Solar Dynamics ◽  
Mass Ejection

Aims. We investigate the formation times of eruptive magnetic flux ropes relative to the onset of solar eruptions, which is important for constraining models of coronal mass ejection (CME) initiation. Methods. We inspected uninterrupted sequences of 131 Å images that spanned more than eight hours and were obtained by the Atmospheric Imaging Assembly on board the Solar Dynamics Observatory to identify the formation times of hot flux ropes that erupted in CMEs from locations close to the limb. The appearance of the flux ropes as well as their evolution toward eruptions were determined using morphological criteria. Results. Two-thirds (20/30) of the flux ropes were formed well before the onset of the eruption (from 51 min to more than eight hours), and their formation was associated with the occurrence of a confined flare. We also found four events with preexisting hot flux ropes whose formations occurred a matter of minutes (from three to 39) prior to the eruptions without any association with distinct confined flare activity. Six flux ropes were formed once the eruptions were underway. However, in three of them, prominence material could be seen in 131 Å images, which may indicate the presence of preexisting flux ropes that were not hot. The formation patterns of the last three groups of hot flux ropes did not show significant differences. For the whole population of events, the mean and median values of the time difference between the onset of the eruptive flare and the appearance of the hot flux rope were 151 and 98 min, respectively. Conclusions. Our results provide, on average, indirect support for CME models that involve preexisting flux ropes; on the other hand, for a third of the events, models in which the ejected flux rope is formed during the eruption appear more appropriate.

scholarly journals Dual-spacecraft observation of large-scale magnetic flux ropes in the Martian ionosphere

2011 ◽  
Vol 116 (A2) ◽  
pp. n/a-n/a ◽  
Author(s):  
D. D. Morgan ◽  
D. A. Gurnett ◽  
F. Akalin ◽  
D. A. Brain ◽  
J. S. Leisner ◽  
...  
Keyword(s):  
Magnetic Flux ◽  
Large Scale ◽  
Magnetic Flux Ropes ◽  
Flux Ropes ◽  
Martian Ionosphere

scholarly journals Understanding the Twist Distribution Inside Magnetic Flux Ropes by Anatomizing an Interplanetary Magnetic Cloud

2018 ◽  
Vol 123 (5) ◽  
pp. 3238-3261 ◽  
Author(s):  
Yuming Wang ◽  
Chenglong Shen ◽  
Rui Liu ◽  
Jiajia Liu ◽  
Jingnan Guo ◽  
...  
Keyword(s):  
Magnetic Flux ◽  
Magnetic Cloud ◽  
Magnetic Flux Ropes ◽  
Flux Ropes

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.

scholarly journals Investigating 1st and 2nd order Fermi acceleration of energetic particles by small-scale magnetic flux ropes at 1AU

2020 ◽  
Vol 1620 ◽  
pp. 012008
Author(s):  
J A le Roux ◽  
G M Webb ◽  
O V Khabarova ◽  
K T Van Eck ◽  
L-L Zhao ◽  
...  
Keyword(s):  
Magnetic Flux ◽  
Energetic Particles ◽  
Small Scale ◽  
Fermi Acceleration ◽  
Magnetic Flux Ropes ◽  
Flux Ropes

scholarly journals Editorial: Magnetic Flux Ropes: From the Sun to the Earth and Beyond

2020 ◽  
Vol 7 ◽  
Author(s):  
Rui Liu ◽  
Jie Zhang ◽  
Yuming Wang ◽  
Hongqiang Song
Keyword(s):  
Magnetic Flux ◽  
The Sun ◽  
Magnetic Flux Ropes ◽  
The Earth ◽  
Flux Ropes
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