Uncovering the process that transports magnetic helicity to coronal mass ejection flux ropes

AbstractFollowing the first observational study of the interaction between two distinct filaments (Su et al. 2007; hereafter, event 1), we present another interesting case observed by SMART telescope on 2005 June 25 with higher spatial resolution (hereafter, event 2). The two events are compared with each other. In event 1 the two filaments erupted subsequently and obvious mass flow was observed to be transferred from one erupting filament to one stable filament which triggered its eruption. On the contrary, in event 2, the two filaments erupted simultaneously and there was no transfer of material noticed between them during the initial stage. The two filaments merged together along the ejection path, indicating the bodily coalesce between the two interacting flux ropes. Moreover, event 1 was associated with a coronal mass ejection (CME), while event 2 was a failed filament eruption, thus without CME association.

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The birth of a coronal mass ejection

Science Advances ◽

10.1126/sciadv.aau7004 ◽

2019 ◽

Vol 5 (3) ◽

pp. eaau7004 ◽

Cited By ~ 11

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.

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

10.5194/egusphere-egu2020-8398 ◽

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.&#160;The model assumes an empirically motivated torus-like flux rope structure that expands self-similarly and contains an embedded analytical magnetic field.&#160;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&#160;and furthermore reconstruct the global flux rope geometry.</p>

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