On the Magnetic Flux Budget in Low‐Corona Magnetic Reconnection and Interplanetary Coronal Mass Ejections

Qiu, Jiong; Hu, Qiang; Howard, T. A.; Yurchyshyn, Vasyl

doi:10.1086/512060

Cited by 283 publications

(389 citation statements)

References 102 publications

(130 reference statements)

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“…Following our discussion on the formation of the dimmings for this event via secondary reconnections with the surrounding fields, it is therefore not possible to directly compare the flux in the MC to the flux in the dimmings. Qiu et al (2007) have computed the flux swept out by flare ribbons for this event and found a value of (18.8 ± 1.8) × 10 21 Mx, which is in good agreement with the total MC flux.…”

Section: Overview Of Three Events With Different Characteristicssupporting

confidence: 68%

See 1 more Smart Citation

The link between CME-associated dimmings and interplanetary magnetic clouds

Mandrini¹,

Nakwacki²,

Attrill

et al. 2008

Proc. IAU

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Abstract. Coronal dimmings often develop in the vicinity of erupting magnetic configurations. It has been suggested that they mark the location of the footpoints of ejected flux ropes and, thus, their magnetic flux can be used as a proxy for the ejected flux. If so, this quantity can be compared to the flux in the associated interplanetary magnetic cloud (MC) to find clues about the origin of the ejected flux rope. In the context of this interpretation, we present several events for which we have done a comparative solar-interplanetary analysis. We combine SOHO/Extreme Ultraviolet Imaging Telescope (EIT) data and Michelson Doppler Imager (MDI) magnetic maps to identify and measure the flux in the dimmed regions. We model the associated MCs and compute their magnetic flux using in situ observations. We find that the magnetic fluxes in the dimmings and MCs are compatible in some events; though this is not the case for large-scale and intense eruptions that occur in regions that are not isolated from others. We conclude that, in these particular cases, a fraction of the dimmed regions can be formed by reconnection between the erupting field and the surrounding magnetic structures, via a stepping process that can also explain other CME associated events.

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Section: Overview Of Three Events With Different Characteristicssupporting

confidence: 68%

“…This indicates that the ejected rope was mostly formed by magnetic reconnection during the eruption process. Qiu et al (2007) found a different result concerning the flux in coronal dimming regions. These authors concluded that the flux in dimming regions is comparable in order of magnitude to the axial MC flux.…”

Section: Discussionmentioning

confidence: 89%

The link between CME-associated dimmings and interplanetary magnetic clouds

Mandrini¹,

Nakwacki²,

Attrill

et al. 2008

Proc. IAU

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“…However, much of this flux is added to the rope by reconnection after the launch of the CME (Qiu et al 2007). Therefore, these observations do not provide conclusive evidence of the partition between axial and poloidal flux in the rope at the onset of the eruption.…”

Section: Magnetic Flux Budgetmentioning

confidence: 99%

“…Webb et al 2000;Mandrini et al 2005;Attrill et al 2006;Jian et al 2006). However, the erupting stucture is strongly modified by magnetic reconnection that occurs in the current sheet under the rising flux rope and produces the post-eruption flare arcade (e.g., Qiu et al 2007). We rather use flux cancellation in the active region to study the flux content of the structure before the eruption onset.…”

Section: Introductionmentioning

confidence: 99%

Photospheric flux cancellation and associated flux rope formation and eruption

Green

Kliem

Wallace

2010

A&A

207

241

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Aims. We study an evolving bipolar active region that exhibits flux cancellation at the internal polarity inversion line, the formation of a soft X-ray sigmoid along the inversion line and a coronal mass ejection. The aim is to investigate the quantity of flux cancellation that is involved in flux rope formation in the time period leading up to the eruption. Methods. The active region is studied using its extreme ultraviolet and soft X-ray emissions as it evolves from a sheared arcade to flux rope configuration. The evolution of the photospheric magnetic field is described and used to estimate how much flux is reconnected into the flux rope. Results. About one third of the active region flux cancels at the internal polarity inversion line in the 2.5 days leading up to the eruption. In this period, the coronal structure evolves from a weakly to a highly sheared arcade and then to a sigmoid that crosses the inversion line in the inverse direction. These properties suggest that a flux rope has formed prior to the eruption. The amount of cancellation implies that up to 60% of the active region flux could be in the body of the flux rope. We point out that only part of the cancellation contributes to the flux in the rope if the arcade is only weakly sheared, as in the first part of the evolution. This reduces the estimated flux in the rope to ∼30% or less of the active region flux. We suggest that the remaining discrepancy between our estimate and the limiting value of ∼10% of the active region flux, obtained previously by the flux rope insertion method, results from the incomplete coherence of the flux rope, due to nonuniform cancellation along the polarity inversion line. A hot linear feature is observed in the active region which rises as part of the eruption and then likely traces out the field lines close to the axis of the flux rope. The flux cancellation and changing magnetic connections at one end of this feature suggest that the flux rope reaches coherence by reconnection immediately before and early in the impulsive phase of the associated flare. The sigmoid is destroyed in the eruption but reforms quickly, with the amount of cancellation involved being much smaller than in the course of its original formation.

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“…Such studies of rapid reconnection during flares, in particular those using the evolution of flare ribbons overlaid on cotemporal magnetograms (Forbes and Priest, 1984;Poletto and Kopp, 1986;Fletcher and Hudson, 2001;Qiu et al, 2002;Qiu et al, 2007;Longcope et al, 2007;Qiu, 2009;Longcope et al, 2010;Kazachenko et al, 2010;Kazachenko et al, 2012), are the most direct antecedents of the present study. These two-ribbon flares generally follow the standard CSHKP flare model (See Priest and Forbes, 2002 for a review).…”

Section: Introductionmentioning

confidence: 72%

Quiescent Reconnection Rate Between Emerging Active Regions and Preexisting Field, with Associated Heating: NOAA AR 11112

et al. 2014

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When magnetic flux emerges from beneath the photosphere it displaces the preexisting field in the corona, and a current sheet generally forms at the boundary between the old and new magnetic domains. Reconnection in the current sheet relaxes this highly stressed configuration to a lower energy state. This scenario is most familiar, and most often studied, in flares, where the flux transfer is rapid. We present here a study of steady, quiescent flux transfer occurring at a rate three orders of magnitude below that in a large flare. In particular we quantify the reconnection rate, and related energy release, occurring as new polarity emerges to form Active Region 11112 (SOL16 October 2010T00:00:00L205C117) within a region of preexisting flux. A bright, low lying kernel of coronal loops above the emerging polarity, observed with the Atmospheric Imaging Assembly onboard the Solar Dynamics Observatory and the X-ray Telescope onboard Hinode, originally shows magnetic connectivity only between regions of newly emerged flux when overlaid on magnetograms from the Helioseisimic and Magnetic Imager. Over the course of several days, this bright kernel advances into the preexisting flux. The advancement of an easily visible boundary into the old flux regions allows measurement of the rate of reconnection between old and new magnetic domains. We compare the reconnection rate to the inferred heating of the coronal plasma. To our knowledge, this is the first measurement of steady, quiescent heating related to reconnection. We determine that the newly emerged flux reconnects at a fairly steady rate of 0.38 × 10 16 Mx s −1 over two days, while the radiated power varies between (2 ∼ 8) × 10 25 erg s −1 over the same time. We find that as much as 40% of the total emerged flux at any given time may have reconnected. The total amount of transferred flux (∼ 1 × 10 21 Mx) and radiated energy (∼ 7.2 × 10 30 ergs) are comparable to that of a large M-or small X-class flare, but are stretched out over 45 hours.

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On the Magnetic Flux Budget in Low‐Corona Magnetic Reconnection and Interplanetary Coronal Mass Ejections

Cited by 283 publications

References 102 publications

The link between CME-associated dimmings and interplanetary magnetic clouds

The link between CME-associated dimmings and interplanetary magnetic clouds

Photospheric flux cancellation and associated flux rope formation and eruption

Quiescent Reconnection Rate Between Emerging Active Regions and Preexisting Field, with Associated Heating: NOAA AR 11112

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