scholarly journals The birth of a coronal mass ejection

2019 ◽  
Vol 5 (3) ◽  
pp. eaau7004 ◽  
Author(s):  
Tingyu Gou ◽  
Rui Liu ◽  
Bernhard Kliem ◽  
Yuming Wang ◽  
Astrid M. Veronig
Keyword(s):  
Magnetic Reconnection ◽  
Coronal Mass Ejection ◽  
Current Sheet ◽  
Magnetic Structure ◽  
Coronal Mass Ejections ◽  
Flux Rope ◽  
Evolutionary Path ◽  
X Ray ◽  
Flux Ropes ◽  
Mass Ejection

The Sun’s atmosphere is frequently disrupted by coronal mass ejections (CMEs), coupled with flares and energetic particles. The coupling is usually attributed to magnetic reconnection at a vertical current sheet connecting the flare and CME, with the latter embedding a helical magnetic structure known as flux rope. However, both the origin of flux ropes and their nascent paths toward eruption remain elusive. Here, we present an observation of how a stellar-sized CME bubble evolves continuously from plasmoids, mini flux ropes that are barely resolved, within half an hour. The eruption initiates when plasmoids springing from a vertical current sheet merge into a leading plasmoid, which rises at increasing speeds and expands impulsively into the CME bubble, producing hard x-ray bursts simultaneously. This observation illuminates a complete CME evolutionary path capable of accommodating a wide variety of plasma phenomena by bridging the gap between microscale and macroscale dynamics.

scholarly journals Observations of flux rope formation prior to coronal mass ejections

2013 ◽  
Vol 8 (S300) ◽  
pp. 209-214 ◽  
Author(s):  
Lucie M. Green ◽  
Bernhard Kliem
Keyword(s):  
Magnetic Flux ◽  
Magnetic Structure ◽  
Solar Atmosphere ◽  
Coronal Mass Ejections ◽  
Flux Rope ◽  
Active Regions ◽  
Magnetic Configuration ◽  
Magnetic Flux Rope ◽  
Source Regions ◽  
Flux Ropes

AbstractUnderstanding the magnetic configuration of the source regions of coronal mass ejections (CMEs) is vital in order to determine the trigger and driver of these events. Observations of four CME productive active regions are presented here, which indicate that the pre-eruption magnetic configuration is that of a magnetic flux rope. The flux ropes are formed in the solar atmosphere by the process known as flux cancellation and are stable for several hours before the eruption. The observations also indicate that the magnetic structure that erupts is not the entire flux rope as initially formed, raising the question of whether the flux rope is able to undergo a partial eruption or whether it undergoes a transition in specific flux rope configuration shortly before the CME.

scholarly journals MODELING UV AND X-RAY EMISSION IN A POST-CORONAL MASS EJECTION CURRENT SHEET

2010 ◽  
Vol 722 (1) ◽  
pp. 625-641 ◽  
Author(s):  
Yuan-Kuen Ko ◽  
John C. Raymond ◽  
Bojan Vršnak ◽  
Eugen Vujić
Keyword(s):  
Coronal Mass Ejection ◽  
Current Sheet ◽  
X Ray ◽  
Mass Ejection

Direct evidence of secondary reconnection inside filamentary currents of magnetic flux ropes in magnetic reconnection

2020 ◽  
Author(s):  
Shimou Wang ◽  
Quanming Lu
Keyword(s):  
Energy Dissipation ◽  
Magnetic Flux ◽  
Magnetic Reconnection ◽  
Current Sheet ◽  
Magnetic Energy ◽  
Flux Rope ◽  
Plasma Jets ◽  
Magnetic Flux Ropes ◽  
Flux Ropes ◽  
Reconnecting Current Sheet

<p>Magnetic reconnection is a fundamental plasma process, by which magnetic energy is explosively released in the current sheet to energize charged particles and to create bi-directional Alfvénic plasma jets. A long-outstanding issue is how the stored magnetic energy is rapidly released in the process. Numerical simulations and observations show that formation and interaction of magnetic flux ropes dominate the evolution of the reconnecting current sheet. Accordingly, most volume of the reconnecting current sheet is occupied by the flux ropes and energy dissipation primarily occurs along their edges via the flux rope coalescence. Here, for the first time, we present in-situ evidence of magnetic reconnection inside the filamentary currents which was driven possibly by electron vortices inside the flux ropes. Our results reveal an important new way for energy dissipation in magnetic reconnection.</p>

Observations of an Electron-only Magnetic Reconnection within a macroscopic Flux Rope in the Magnetotail

2020 ◽  
Author(s):  
Hengyan Man ◽  
Meng Zhou ◽  
Yongyuan Yi ◽  
Zhihong Zhong ◽  
Xiaohua Deng
Keyword(s):  
Electric Field ◽  
Magnetic Reconnection ◽  
Current Sheet ◽  
Large Scale ◽  
Energy Transport ◽  
Flux Rope ◽  
Space Plasmas ◽  
Positive Energy ◽  
Guide Field ◽  
Flux Ropes

<p>It is widely accepted that flux ropes play important roles in the momentum and energy transport in space plasmas. Recent observations found that magnetic reconnection occurs at the interface between two counter flows around the center of flux ropes. In this presentation, we report a novel observation by MMS that reconnection occurs at the edge of a large-scale flux rope, the cross-section of which was about 2.5 Re. The flux rope was observed at the dusk side in Earth’s magnetotail and was highly oblique with its axis proximity along the X<sub>GSM</sub> direction. We found an electron-scale current sheet near the edge of this flux rope. The Hall magnetic and electric field, super-Alfvénic electron outflow, parallel electric field and positive energy dissipation were observed associated with the current sheet. All the above signatures indicate that MMS detected a reconnecting current sheet in the presence of a large guide field. Interestingly, ions were not coupled in this reconnection, akin to the electron-only reconnection observed in the magnetosheath turbulence. We suggest that the electron-scale current sheet was caused by the strong magnetic field perturbation inside the flux rope. This result will shed new lights for understanding the multi-scale coupling associated with flux ropes in space plasmas.</p>

Modelling coronal mass ejection flux ropes signatures using Approximate Bayesian Computation: applications to Parker Solar Probe

2020 ◽  
Author(s):  
Andreas Weiss ◽  
Christian Möstl ◽  
Teresa Nieves-Chinchilla ◽  
Tanja Amerstorfer ◽  
Erika Palmerio ◽  
...  
Keyword(s):  
Magnetic Field ◽  
Coronal Mass Ejection ◽  
Approximate Bayesian Computation ◽  
Flux Rope ◽  
Bayesian Computation ◽  
Abc Algorithm ◽  
Flux Ropes ◽  
Approximate Bayesian ◽  
Mass Ejection

<p>We present an updated three-dimensional coronal rope ejection (3DCORE) model and an associated pipeline that is capable of producing extremely large ensembles of synthetic in-situ magnetic field measurements from simulated coronal mass ejection flux ropes. The model assumes an empirically motivated torus-like flux rope structure that expands self-similarly and contains an embedded analytical magnetic field. Using an Approximate Bayesian computation (ABC) algorithm we validate the model by showing that it is capable of qualitatively reproducing measured flux rope signatures. The ABC algorithm also gives us uncertainty estimates in the form of probability distributions for all model parameters. We show the first results for applying our model and algorithms to coronal mass ejections observed in situ by Parker Solar Probe, specifically the event on 2018 November 12 at 0.26AU, where we attempt to reproduce the measured magnetic field signatures and furthermore reconstruct the global flux rope geometry.</p>

scholarly journals X-RAY EMISSION FROM THE BASE OF A CURRENT SHEET IN THE WAKE OF A CORONAL MASS EJECTION

2009 ◽  
Vol 699 (1) ◽  
pp. 245-253 ◽  
Author(s):  
P. Saint-Hilaire ◽  
S. Krucker ◽  
R.P. Lin
Keyword(s):  
Coronal Mass Ejection ◽  
Current Sheet ◽  
X Ray ◽  
Mass Ejection ◽  
A Current

Flux Rope Model of the 2003 October 28–30 Coronal Mass Ejection and Interplanetary Coronal Mass Ejection

2006 ◽  
Vol 642 (1) ◽  
pp. 541-553 ◽  
Author(s):  
J. Krall ◽  
V. B. Yurchyshyn ◽  
S. Slinker ◽  
R. M. Skoug ◽  
J. Chen
Keyword(s):  
Coronal Mass Ejection ◽  
Flux Rope ◽  
Interplanetary Coronal Mass Ejection ◽  
Mass Ejection

scholarly journals Photospheric magnetic field of an eroded-by-solar-wind coronal mass ejection

2016 ◽  
Vol 12 (S327) ◽  
pp. 67-70
Author(s):  
J. Palacios ◽  
C. Cid ◽  
E. Saiz ◽  
A. Guerrero
Keyword(s):  
Magnetic Field ◽  
Solar Wind ◽  
Coronal Mass Ejection ◽  
Coronal Hole ◽  
Interplanetary Medium ◽  
Flux Rope ◽  
Magnetic Characteristics ◽  
Interplanetary Coronal Mass Ejection ◽  
Fast Wind ◽  
Mass Ejection

AbstractWe have investigated the case of a coronal mass ejection that was eroded by the fast wind of a coronal hole in the interplanetary medium. When a solar ejection takes place close to a coronal hole, the flux rope magnetic topology of the coronal mass ejection (CME) may become misshapen at 1 AU as a result of the interaction. Detailed analysis of this event reveals erosion of the interplanetary coronal mass ejection (ICME) magnetic field. In this communication, we study the photospheric magnetic roots of the coronal hole and the coronal mass ejection area with HMI/SDO magnetograms to define their magnetic characteristics.

Radio and X‐Ray Studies of a Coronal Mass Ejection Associated with a Very Slow Prominence Eruption

1997 ◽  
Vol 475 (1) ◽  
pp. 348-360 ◽  
Author(s):  
N. Gopalswamy ◽  
Y. Hanaoka ◽  
M. R. Kundu ◽  
S. Enome ◽  
J. R. Lemen ◽  
...  
Keyword(s):  
Coronal Mass Ejection ◽  
X Ray ◽  
Mass Ejection
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