Physical Processes Involved in the EUV “Surge” Event of 9 May 2012

Fuentes, M. C. López; Mandrini, C. H.; Poisson, Mariano; Démoulin, P.; Cristiani, G.; López, Fernando Manuel; Luoni, M. L.

doi:10.1007/s11207-018-1384-4

Cited by 9 publications

(18 citation statements)

References 81 publications

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“…We show quantitative evidence of flux cancellation in seven cases, and infer the presence of flux cancellation in other cases based on the observed flux convergence. Although we do not rule out other possibilities, the observations of flux convergence at the base of events suggests that flux cancellation could play an important role in triggering several of these events, in accord with many recent similar findings of flux cancellation leading to jet eruptions (Huang et al 2015;Panesar et al 2016Panesar et al , 2017Tiwari et al 2016Tiwari et al , 2018Sterling et al 2017Sterling et al , 2018Panesar et al 2018a;López Fuentes et al 2018). As was first proposed by van Ballegooijen & Martens (1989) and Moore & Roumeliotis (1992), and has been observationally confirmed (e.g., Panesar et al 2016Panesar et al , 2017Panesar et al , 2018aTiwari et al 2018;Sterling et al 2018;Chintzoglou et al 2019), the process of flux cancellation (driven by converging photospheric flows) can prepare and trigger the magnetic field that explodes in a flare eruption.…”

Section: (A)supporting

confidence: 89%

Fine-scale Explosive Energy Release at Sites of Prospective Magnetic Flux Cancellation in the Core of the Solar Active Region Observed by Hi-C 2.1, IRIS, and SDO

Tiwari¹,

Panesar²,

Moore³

et al. 2019

ApJ

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The second Hi-C flight (Hi-C2.1) provided unprecedentedly-high spatial and temporal resolution (∼250km, 4.4s) coronal EUV images of Fe IX/X emission at 172Å, of AR 12712 on 29-May-2018, during 18:56:21-19:01:56 UT. Three morphologically-different types (I: dot-like, II: loop-like, III: surge/jetlike) of fine-scale sudden-brightening events (tiny microflares) are seen within and at the ends of an arch filament system in the core of the AR. Although type Is (not reported before) resemble IRIS-bombs (in size, and brightness wrt surroundings), our dot-like events are apparently much hotter, and shorter in span (70s). We complement the 5-minute-duration Hi-C2.1 data with SDO/HMI magnetograms, SDO/AIA EUV images, and IRIS UV spectra and slit-jaw images to examine, at the sites of these events, brightenings and flows in the transition-region and corona and evolution of magnetic flux in the photosphere. Most, if not all, of the events are seated at sites of opposite-polarity magnetic flux convergence (sometimes driven by adjacent flux emergence), implying likely flux cancellation at the microflare's polarity inversion line. In the IRIS spectra and images, we find confirming evidence of field-aligned outflow from brightenings at the ends of loops of the arch filament system. In types I and II the explosion is confined, while in type III the explosion is ejective and drives jet-like outflow. The light-curves from Hi-C, AIA and IRIS peak nearly simultaneously for many of these events and none of the events display a systematic cooling sequence as seen in typical coronal flares, suggesting that these tiny brightening-events have chromospheric/transition-region origin.

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Section: (A)supporting

confidence: 89%

Fine-scale Explosive Energy Release at Sites of Prospective Magnetic Flux Cancellation in the Core of the Solar Active Region Observed by Hi-C 2.1, IRIS, and SDO

Tiwari¹,

Panesar²,

Moore³

et al. 2019

ApJ

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“…We obtained this velocity by tracking the front along successive images and then computing the slope of the position versus time curve, from the original filament location to the farthest position reached by the surge front. Although this velocity is higher than the 190 km s −1 obtained for the 12:23 UT surge studied by López Fuentes et al (2018), it is still within the usual values observed in this kind of events (Raouafi et al, 2016). Figure 6b).…”

Section: Uv Continuum and Euv Evolution As Seen From Earthsupporting

confidence: 57%

“…The magnetic evolution of AR 11476 from appearance, on the eastern solar limb, on 04 May 2012 until the end of 10 May has been discussed in detail by López Fuentes et al (2018). We summarize here their main results.…”

Section: Summary Of the Photospheric Magnetic Field Evolutionmentioning

confidence: 93%

“…Each arrow is accompanied by labels indicating the X-ray class and time of the flares. As a reference we identify the peak of the event at 12:23 UT that was studied by López Fuentes et al (2018) and that of the event at 4:18 UT studied by Yang and Zhang (2018). The peak between the C1.6 and M4.1 flares, indicated with a red arrow, corresponds to a flare associated to the neighboring jet that occurred next to AR 11576 to the east at 20:45 UT and that is mentioned in Section 2.3.…”

Section: Summary Of the Photospheric Magnetic Field Evolutionmentioning

confidence: 99%

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Two successive partial mini-filament confined ejections

Poisson

Bustos

Fuentes

et al. 2020

Advances in Space Research

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Active region (AR) NOAA 11476 produced a series of confined plasma ejections, mostly accompanied by flares of X-ray class M, from 08 to 10 May 2012. The structure and evolution of the confined ejections resemble that of EUV surges; however, their origin is associated to the destabilization and eruption of a mini-filament, which lay along the photospheric inversion line (PIL) of a large rotating bipole. Our analysis indicate that the bipole rotation and flux cancellation along the PIL have a main role in destabilizing the structure and triggering the ejections. The observed bipole emerged within the main following AR polarity. Previous studies have analyzed and discussed in detail two events of this series in which the mini-filament erupted as a whole, one at 12:23 UT on 09 May and the other at 04:18 UT on 10 May. In this article we present the observations of the confined eruption and M4.1 flare on 09 May 2012 at 21:01 UT (SOL2012-05-09T21:01:00) and the previous activity in which the mini-filament was involved. For the analysis we use data in multiple wavelengths (UV, EUV, X-rays, and magnetograms) from space instruments. In this particular case, the mini-filament is seen to erupt in two different sections. The northern section erupted accompanied by a C1.6 flare and the southern section did it in association with the M4.1 flare. The global structure and direction of both confined ejections and the location of a far flare kernel, to where the plasma is seen to flow, suggest that both ejections and flares follow a similar underlying mechanism.

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“…López Fuentes et al (2000) reported their existence for the first time in a rotating bipolar AR and they were later observed in many other examples (see e.g. Luoni et al 2011;Mandrini et al 2014;Valori et al 2015;Yardley et al 2016;Vemareddy & Démoulin 2017;Dacie et al 2018;López Fuentes et al 2018). They also have been found in numerical simulations of emerging FRs (Archontis & Hood 2010;Cheung et al 2010;MacTaggart 2011;Jouve et al 2013;Rempel & Cheung 2014;Takasao et al 2015).…”

Section: Introductionmentioning

confidence: 89%

Correcting the effect of magnetic tongues on the tilt angle of bipolar active regions

Poisson

Fuentes

Mandrini

et al. 2020

A&A

Self Cite

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Context. The magnetic polarities of bipolar active regions (ARs) exhibit elongations in line-of-sight magnetograms during their emergence. These elongations are referred to as magnetic tongues and attributed to the presence of twist in the emerging magnetic flux-ropes (FRs) that form ARs. Aims. The presence of magnetic tongues affects the measurement of any AR characteristic that depends on its magnetic flux distribution. The AR tilt-angle is one of them. We aim to develop a method to isolate and remove the flux associated with the tongues to determine the AR tilt-angle with as much precision as possible. Methods. As a first approach, we used a simple emergence model of a FR. This allowed us to develop and test our aim based on a method to remove the effects of magnetic tongues. Then, using the experience gained from the analysis of the model, we applied our method to photospheric observations of bipolar ARs that show clear magnetic tongues. Results. Using the developed procedure on the FR model, we can reduce the deviation in the tilt estimation by more than 60%. Next we illustrate the performance of the method with four examples of bipolar ARs selected for their large magnetic tongues. The new method efficiently removes the spurious rotation of the bipole. This correction is mostly independent of the method input parameters and significant since it is larger than all the estimated tilt errors. Conclusions. We have developed a method to isolate the magnetic flux associated with the FR core during the emergence of bipolar ARs. This allows us to compute the AR tilt-angle and its evolution as precisely as possible. We suggest that the high dispersion observed in the determination of AR tilt-angles in studies that massively compute them from line-of sight magnetograms can be partly due to the existence of magnetic tongues whose presence is not sufficiently acknowledged.

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Physical Processes Involved in the EUV “Surge” Event of 9 May 2012

Cited by 9 publications

References 81 publications

Fine-scale Explosive Energy Release at Sites of Prospective Magnetic Flux Cancellation in the Core of the Solar Active Region Observed by Hi-C 2.1, IRIS, and SDO

Fine-scale Explosive Energy Release at Sites of Prospective Magnetic Flux Cancellation in the Core of the Solar Active Region Observed by Hi-C 2.1, IRIS, and SDO

Two successive partial mini-filament confined ejections

Correcting the effect of magnetic tongues on the tilt angle of bipolar active regions

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