The Coronal‐dimming Footprint of a Streamer‐Puff Coronal Mass Ejection: Confirmation of the Magnetic‐Arch‐Blowout Scenario

Moore, Ronald L.; Sterling, Alphonse C.

doi:10.1086/516620

Cited by 47 publications

(26 citation statements)

References 33 publications

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“…They tend to lie in CRRs and, in those cases where higher-resolution magnetometer data was examined, it seems like there is no CS. In the context of the hypothesis presented here, the locations of these CRRs is consistent with their origin in ''pseudo-streamers'', those streamers which overlie twin loop arcades and separate coronal holes of the same polarity [Wang et al, 2007;Moore and Sterling, 2007]. In the context of the model in Figure 1, the physics of the streamer does not change at all because the confinement is due to external magnetic pressure.…”

Section: Streamer Origins Of Slow Windsupporting

confidence: 71%

Quiescent current sheets in the solar wind and origins of slow wind

Suess

Steiger

et al. 2009

J. Geophys. Res.

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[1] Solar wind near the heliospheric current sheet is investigated using Ulysses and ACE data in a superposed epoch analysis for several days on either side of the current sheets. Only data near sunspot minima are used, minimizing the influence of transients. New results are shown for composition and ionization state. Existing results showing a $2 day wide depletion in He/H (He ++ /H + ) at the current sheet are confirmed, although the depletion is generally more narrow. A recent finding of a broad 5-10 day wide reduction in He/H around the current sheet is also confirmed. An important result is that the narrow depletion is not a real phenomenon but is instead a statistical consequence of the superposition of transient depletions that also create the broad reduction in the averages. These transient depletions last from a few hours up to several days, come from the core of streamers, and are embedded in a quasi-steady flow from streamers' legs. Most depletions contain a current sheet just inside one edge, leading to the apparent narrow depletion at the current sheet in the superposed epoch analysis. These results lead us to a hypothesis for how the He/H depletions form with a current sheet just inside one edge. Fe/O fluctuations associated with the He/H fluctuations further show that mixing of plasma from coronal holes adjacent to streamer brightness boundaries into outflow inside the brightness boundary is not an important process.

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Section: Streamer Origins Of Slow Windsupporting

confidence: 71%

Quiescent current sheets in the solar wind and origins of slow wind

Suess

Steiger

et al. 2009

J. Geophys. Res.

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“…Moreover, it is possible that the radial eruption of the sheared structure met with the EUV loops and guided by the loops, which lead to produce the non-radial CME. The situation is consistent with the magnetic-arch-blowout scenario for over-and-out CMEs proposed by Bemporad et al (2005) and Moore and Sterling (2007).…”

Section: Conclusion and Discussionsupporting

confidence: 90%

The coronal mass ejection associated with the loop eruption and coronal dimmings on 2009 December 13

Zheng

Jiang

Yang

et al. 2010

Astrophys Space Sci

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By using the multi-wavelength observations from the Solar Terrestrial Relations Observatory (STEREO), the Solar and Heliospheric Observatory (SOHO), the Transition Region and Coronal Explorer (TRACE) and the HIN-ODE, we study a coronal mass ejection (CME) and associated coronal dimming occurred on 2009 December 13, as a consequence of the expansion and eruption of EUV loops. The activities were probably triggered by the new flux emergence and the convergence motions, which were evident in the magnetograms from Michelson Doppler Imager (MDI) on the SOHO. The emergence led to the destabilization and eruption of the preexistent flux rope, which was highly-sheared over the polarity inversion line. Driven by the ejection of the flux rope, the overlying loops initially slowly rose and then erupted. As a result, two coronal dimming regions formed at the footprints of the loops and a B1.9 flare, about half an hour later, occurred in the eruptive region near one foot of the eruptive loops. The CME had a very close temporal and spatial relationship to the expanding loops, and it is very likely that the CME directly developed from the eruptive loops. The CME mass calculated from the EUV dimming was of the same order of the typical CME mass, suggesting that the dimming region supplied major of the mass for the CME. The kinematic evolution of the CME was basically consistent with the three-phases scenario: the initiation phase, impulsive acceleration phase, and propagation phase. The onset of the CME could be well explained by the emerging flux trigger mechanism.

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“…Moreover, inspection of the full-frame EUVI images show that weaker dimmings grow to cover an even larger extent than shown here. This sort of large-scale eruption with a more localized flaring region has now been detailed for several cases (e.g., Gopalswamy & Thompson 2000;Wang et al 2002;Sterling & Moore 2004;Attrill et al 2008;Moore & Sterling 2007).…”

Section: Euv Trace and Stereo Observations Of The Eruptionmentioning

confidence: 99%

Evidence for magnetic flux cancelation leading to an ejective solar eruption observed byHinode,TRACE,STEREO, andSoHO/MDI

Sterling¹,

Chifor²,

Mason³

et al. 2010

A&A

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Aims. We study the onset of a solar eruption involving a filament ejection on 2007 May 20. Methods. We observe the filament in Hα images from Hinode/SOT and in EUV with TRACE and STEREO/SECCHI/EUVI. Hinode/XRT images are used to study the eruption in soft X-rays. From spectroscopic data taken with Hinode/EIS we obtain bulkflow velocities, line profiles, and plasma densities in the onset region. The magnetic field evolution was observed in SoHO/MDI magnetograms. Results. We observed a converging motion between two opposite polarity sunspots that form the primary magnetic polarity inversion line (PIL), along which resides filament material before eruption. Positive-flux magnetic elements, perhaps moving magnetic features (MMFs) flowing from the spot region, appear north of the spots, and the eruption onset occurs where these features cancel repeatedly in a negative-polarity region north of the sunspots. An ejection of material observed in Hα and EUV marks the start of the filament eruption (its "fast-rise"). The start of the ejection is accompanied by a sudden brightening across the PIL at the jet's base, observed in both broad-band images and in EIS. Small-scale transient brightenings covering a wide temperature range (Log T e = 4.8−6.3) are also observed in the onset region prior to eruption. The preflare transient brightenings are characterized by sudden, localized density enhancements (to above Log n e [cm −3 ] = 9.75, in Fe xiii) that appear along the PIL during a time when pre-flare brightenings were occurring. The measured densities in the eruption onset region outside the times of those enhancements decrease with temperature.Persistent downflows (red-shifts) and line-broadening (Fe xii) are present along the PIL.Conclusions. The array of observations is consistent with the pre-eruption sheared-core magnetic field being gradually destabilized by evolutionary tether-cutting flux cancelation that was driven by converging photospheric flows, and the main filament ejection being triggered by flux cancelation between the positive flux elements and the surrounding negative field. A definitive statement however on the eruption's ultimate cause would require comparison with simulations, or additional detailed observations of other eruptions occurring in similar magnetic circumstances.

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The Coronal‐dimming Footprint of a Streamer‐Puff Coronal Mass Ejection: Confirmation of the Magnetic‐Arch‐Blowout Scenario

Cited by 47 publications

References 33 publications

Quiescent current sheets in the solar wind and origins of slow wind

Quiescent current sheets in the solar wind and origins of slow wind

The coronal mass ejection associated with the loop eruption and coronal dimmings on 2009 December 13

Evidence for magnetic flux cancelation leading to an ejective solar eruption observed byHinode,TRACE,STEREO, andSoHO/MDI

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