Solar Physics

, 293:166 | Cite as

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

  • Marcelo López FuentesEmail author
  • Cristina H. Mandrini
  • Mariano Poisson
  • Pascal Démoulin
  • Germán Cristiani
  • Fernando M. López
  • Maria Luisa Luoni


We study an extreme ultraviolet (EUV) confined ejection observed on 9 May 2012 in Active Region (AR) NOAA 11476. For the analysis we use observations in multiple wavelengths (EUV, X-rays, H\(\upalpha\), and magnetograms) from a variety of ground- and space-based instruments. The magnetic configuration showed two rotating bipoles within the following polarity of the AR. This evolution was present some tens of hours before the studied event and continued thereafter. During this period, the magnetic flux of both bipoles continuously decreased. A mini-filament with a length of \({\approx}\,30''\) lay along the photospheric inversion line of the largest bipole. The mini-filament was observed to erupt, accompanied by an M4.7 flare (SOL20120509T12:23:00). This injected dense material as well as twist along closed loops in the form of a very broad ejection whose morphology resembled that of typical H\(\upalpha\) surges. We conclude that the flare and eruption can be explained as due to two reconnection processes, one occurring below the erupting mini-filament, and another above it. This second process injects the mini-filament plasma within the reconnected closed loops linking the main AR polarities. By analyzing the magnetic topology using a force-free model of the coronal field, we identify the location of quasi-separatix layers, where reconnection is prone to occur, and present a detailed interpretation of the chromospheric and coronal eruption observations. In particular, this event, in contrast to what has been proposed in several models explaining surges and/or jets, is not produced by magnetic flux emergence, but by magnetic flux cancellation accompanied by the rotation of the bipoles. In fact, the conjunction of these two processes, flux cancellation and bipole rotations, is at the origin of a series of events, homologous to the event we analyze in this article, which occurred in AR 11476 from 8 to 10 May 2012.


Active Regions, Models Flares, Relation to Magnetic Field Magnetic Reconnection, Observational Signatures Surges Jets 



The authors are grateful for the insightful referee, who stimulated us to improve several parts of the manuscript. The authors would like to thank Carlos Francile from the Astronomical Observatory Felix Aguilar, University of San Juan, for his invaluable help in the processing of HASTA data. MLF, CHM and GC are members of the Carrera del Investigador Científico of the Consejo Nacional de Investigaciones Científicas y Técnicas (CONICET) of Argentina. MP and FL are CONICET Fellows. MP, MLF, GC and CHM acknowledge financial support from the Argentinean grants PICT 2012-0973 (ANPCyT), UBACyT 20020130100321 and PIP 2012-01-403 (CONICET).

Disclosure of Potential Conflicts of Interest

The authors declare that they have no conflicts of interest.

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Authors and Affiliations

  1. 1.Instituto de Astronomía y Física del Espacio (IAFE)CONICET-UBABuenos AiresArgentina
  2. 2.Facultad de Ciencias Exactas y Naturales (FCEN)UBABuenos AiresArgentina
  3. 3.LESIA, Observatoire de Paris, Université PSL, CNRS, Sorbonne Université, Univ. Paris DiderotSorbonne Paris CitéParisFrance
  4. 4.Instituto de Ciencias Astronómicas, de la Tierra y del Espacio (ICATE)CONICETSan JuanArgentina

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