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Solar Physics

, 293:42 | Cite as

Analysis of a Failed Eclipse Plasma Ejection Using EUV Observations

  • E. Tavabi
  • S. Koutchmy
  • C. Bazin
Article

Abstract

The photometry of eclipse white-light (W-L) images showing a moving blob is interpreted for the first time together with observations from space with the PRoject for On Board Autonomy (PROBA-2) mission (ESA). An off-limb event seen with great details in W-L was analyzed with the SWAP imager (Sun Watcher using Active pixel system detector and image Processing) working in the EUV near 174 Å. It is an elongated plasma blob structure of 25 Mm diameter moving above the east limb with coronal loops under. Summed and co-aligned SWAP images are evaluated using a 20-h sequence, in addition to the 11 July, 2010 eclipse W-L images taken from several sites. The Atmospheric Imaging Assembly (AIA) instrument on board the Solar Dynamics Observatory (SDO) recorded the event suggesting a magnetic reconnection near a high neutral point; accordingly, we also call it a magnetic plasmoid. The measured proper motion of the blob shows a velocity up to \(12~\mbox{km}\,\mbox{s}^{-1}\). Electron densities of the isolated condensation (cloud or blob or plasmoid) are photometrically evaluated. The typical value is \(10^{8}~\mbox{cm}^{-3}\) at \(r=1.7~\mathrm{R}_{\odot}\), superposed on a background corona of \(10^{7}~\mbox{cm}^{-3}\) density. The mass of the cloud near its maximum brightness is found to be \(1.6\times10^{13}\) g, which is typically \(0.6\times10^{-4}\) of the overall mass of the corona. From the extrapolated magnetic field the cloud evolves inside a rather broad open region but decelerates, after reaching its maximum brightness. The influence of such small events for supplying material to the ubiquitous slow wind is noticed. A precise evaluation of the EUV photometric data, after accurately removing the stray light, suggests an interpretation of the weak 174 Å radiation of the cloud as due to resonance scattering in the Fe IX/X lines.

Keywords

Corona, blob, magnetic reconnections, coronal loops, plasmoid, EUV radiation Resonance scattering Eclipses 

Notes

Acknowledgements

This work has benefited from the SWAP G-I program developed at the ROB; A. De Groof, D. Berghmans, B. Nicula and D. Seaton helped with the preparation of an earlier preliminary report of the SWAP observations. We also thank J. Mouette, J.-M. Lecleire, Ch. Nitschelm and especially M. Druckmuller for providing excellent eclipse images, and L. Golub, V. Slemzin, A. Engel, B. Filippov and Z. Mikic for useful discussions and meaningful suggestions.

Eclipse observations were supported by CNES (France); we thank J.-Y. Prado and P. Martinez for their interest and implication in our work. More discussions and suggestions during the course of this work by Andrei Zhukov, Laurent Dolla, Frederic Auchere, Jean-Claude Vial, Guillaume Aulanier, Jacques Dubeau, A. Urnov, E. Podladchikova, Y-M. Wang and others were greatly appreciated. E.T. is also grateful to the Iran National Foundation INSF. The SDO and the STEREO missions are space missions by NASA.

Disclosure of Potential Conflicts of Interest

The authors declare that they have no conflicts of interest.

Supplementary material

11207_2018_1257_MOESM1_ESM.avi (25.7 mb)
# 1 – The STEREO B 171 Å disk and radially filtered movie of 11 July, 2011 (AVI 25.7 MB)
11207_2018_1257_MOESM2_ESM.avi (25.6 mb)
# 2 – AIA radially filtered movie of July 11, 2011 from 13 UT to 21 UT (AVI 25.6 MB)
11207_2018_1257_MOESM3_ESM.wmv (279 kb)
# 3 – The full FOV movie made from a series of summed over 2 h SWAP EUV images with a cadence of 1 h from 7 h to 23 h shown in log scale (WMV 279 kB)
11207_2018_1257_MOESM4_ESM.mov (6.4 mb)
# 3bis – As movie #3 but using an enhanced contrast to display each frame (MOV 6.4 MB)

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Copyright information

© Springer Science+Business Media B.V., part of Springer Nature 2018

Authors and Affiliations

  1. 1.Institut d’Astrophysique de ParisSorbonne Universités, UMR 7095, CNRS and UPMCParisFrance
  2. 2.Physics DepartmentPayame Noor University (PNU)TehranIran
  3. 3.Research Institute for Applied Physics and Astronomy (RIAPA)University of TabrizTabrizIran
  4. 4.LISE LaboratoryUPMCParisFrance

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