scholarly journals Observation of interactions between two erupting filaments

2009 ◽  
Vol 5 (S264) ◽  
pp. 99-101
Author(s):  
Yu Liu ◽  
Jiangtao Su ◽  
Yuandeng Shen ◽  
Liheng Yang
Keyword(s):  
Observational Study ◽  
Coronal Mass Ejection ◽  
Spatial Resolution ◽  
Mass Flow ◽  
Interesting Case ◽  
Filament Eruption ◽  
Initial Stage ◽  
Flux Ropes ◽  
Mass Ejection

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.

Radio Observations of Rapid Acceleration in a Slow Filament Eruption/Fast Coronal Mass Ejection Event

2004 ◽  
Vol 607 (1) ◽  
pp. 530-539 ◽  
Author(s):  
M. R. Kundu ◽  
S. M. White ◽  
V. I. Garaimov ◽  
P. K. Manoharan ◽  
P. Subramanian ◽  
...  
Keyword(s):  
Coronal Mass Ejection ◽  
Radio Observations ◽  
Filament Eruption ◽  
Mass Ejection ◽  
Ejection Event

scholarly journals Determining the full halo coronal mass ejection characteristics

2008 ◽  
Vol 4 (S257) ◽  
pp. 279-281
Author(s):  
V. G. Fainshtein
Keyword(s):  
Coronal Mass Ejection ◽  
Coronal Mass Ejections ◽  
Radial Direction ◽  
Ice Cream ◽  
The Sun ◽  
Initial Stage ◽  
Halo Coronal Mass Ejection ◽  
Mass Ejection

AbstractIn this paper we determined the parameters of 45 full halo coronal mass ejections (HCMEs) for various modifications of their cone forms (“ice cream cone models”). We show that the CME determined characteristics depend significantly on the CME chosen form. We show that, regardless of the CME chosen form, the trajectory of practically all the considered HCMEs deviate from the radial direction to the Sun-to-Earth axis at the initial stage of their movement.

Failed Filament Eruption Inside a Coronal Mass Ejection in Active Region 11121 (Postprint)

2013 ◽  
Author(s):  
D. Kuridze ◽  
M. Mathioudakie ◽  
A. F. Kowalski ◽  
P. H. Keys ◽  
D. B. Jess ◽  
...  
Keyword(s):  
Active Region ◽  
Coronal Mass Ejection ◽  
Filament Eruption ◽  
Mass Ejection

scholarly journals A STUDY OF A FAILED CORONAL MASS EJECTION CORE ASSOCIATED WITH AN ASYMMETRIC FILAMENT ERUPTION

2013 ◽  
Vol 771 (1) ◽  
pp. 65 ◽  
Author(s):  
Navin Chandra Joshi ◽  
Abhishek K. Srivastava ◽  
Boris Filippov ◽  
Wahab Uddin ◽  
Pradeep Kayshap ◽  
...  
Keyword(s):  
Coronal Mass Ejection ◽  
Filament Eruption ◽  
Mass Ejection

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.

Transequatorial Filament Eruption and Its Link to a Coronal Mass Ejection

2006 ◽  
Vol 6 (2) ◽  
pp. 247-259 ◽  
Author(s):  
Jing-Xiu Wang ◽  
Gui-Ping Zhou ◽  
Ya-Yuan Wen ◽  
Yu-Zong Zhang ◽  
Hua-Ning Wang ◽  
...  
Keyword(s):  
Coronal Mass Ejection ◽  
Filament Eruption ◽  
Mass Ejection

scholarly journals FEATURES OF THE INITIAL STAGE OF FORMATION OF FAST CORONAL MASS EJECTION ON FEBRUARY 25, 2014

2020 ◽  
Vol 6 (3) ◽  
pp. 3-17
Author(s):  
Viktor Eselevich ◽  
Maxim Eselevich
Keyword(s):  
Shock Wave ◽  
Coronal Mass Ejection ◽  
Flux Rope ◽  
Solar Radius ◽  
Magnetic Flux Rope ◽  
Initial Stage ◽  
Frontal Structure ◽  
Explosive Expansion ◽  
Mass Ejection ◽  
Full Pressure

We have analyzed the fast coronal mass ejection (CME) that occurred on February 25, 2014. The analysis is based on images taken in the 131, 211, 304, and 1700 Å UV channels of the SDO/AIA instrument and from observations obtained in the Hα line (6562.8 Å) with the telescopes of the Teide and Big Bear Observatories. The February 25, 2014 CME is associated with the ejection and subsequent explosive expansion of the magnetic flux rope, which appeared near the solar surface presumably due to the tether-cutting magnetic reconnection. The impulse of full pressure (thermal plus magnetic) resulting from such an “explosion” acts on the overlying coronal arcades, causing them to merge and form an accelerated moving frontal structure of the CME. This pressure impulse also generates a blast collisional shock wave ahead of the CME, whose velocity decreases rapidly with distance. At large distances R>7R₀ (R₀ is the solar radius) from the center of the Sun in front of the CME, a shock wave of another type is formed — a “piston” collisional shock wave whose velocity varies little with distance. At R≥15R₀, there is a transition from a collisional to a collisionless shock wave.

scholarly journals Probable detection of an eruptive filament from a superflare on a solar-type star

2021 ◽  
Author(s):  
Kosuke Namekata ◽  
Hiroyuki Maehara ◽  
Satoshi Honda ◽  
Yuta Notsu ◽  
Soshi Okamoto ◽  
...  
Keyword(s):  
Coronal Mass Ejection ◽  
Coronal Mass Ejections ◽  
Spectroscopic Observation ◽  
Type Star ◽  
Filament Eruption ◽  
Radiated Energy ◽  
Solar Type ◽  
Solar Filament ◽  
Mass Ejection ◽  
Solar Type Star

AbstractSolar flares are often accompanied by filament/prominence eruptions (~104 K and ~1010−11 cm−3), sometimes leading to coronal mass ejections that directly affect the Earth’s environment1,2. ‘Superflares’ are found on some active solar-type (G-type main-sequence) stars3–5, but the filament eruption–coronal mass ejection association has not been established. Here we show that our optical spectroscopic observation of the young solar-type star EK Draconis reveals evidence for a stellar filament eruption associated with a superflare. This superflare emitted a radiated energy of 2.0 × 1033 erg, and a blueshifted hydrogen absorption component with a high velocity of −510 km s−1 was observed shortly afterwards. The temporal changes in the spectra strongly resemble those of solar filament eruptions. Comparing this eruption with solar filament eruptions in terms of the length scale and velocity strongly suggests that a stellar coronal mass ejection occurred. The erupted filament mass of 1.1 × 1018 g is ten times larger than those of the largest solar coronal mass ejections. The massive filament eruption and an associated coronal mass ejection provide the opportunity to evaluate how they affect the environment of young exoplanets/the young Earth6 and stellar mass/angular momentum evolution7.

scholarly journals Coronal Mass Ejection: Initiation, Magnetic Helicity, and Flux Ropes. II. Turbulent Diffusion–driven Evolution

2003 ◽  
Vol 595 (2) ◽  
pp. 1231-1250 ◽  
Author(s):  
T. Amari ◽  
J. F. Luciani ◽  
J. J. Aly ◽  
Z. Mikic ◽  
J. Linker
Keyword(s):  
Coronal Mass Ejection ◽  
Turbulent Diffusion ◽  
Magnetic Helicity ◽  
Flux Ropes ◽  
Mass Ejection
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