Initiation of CMEs: The role of magnetic twist
Recent multiwavelength observations, modelling results and theoretical developments indicate the importance of twisted magnetic configurations in solar active regions (ARs) in the initiation of coronal mass ejections (CMEs). Through multiwavelength analysis of a few representative events we make an...
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Elsevier Ltd
2000
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| LEADER | 17907caa a22013337a 4500 | ||
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| 001 | PAPER-21078 | ||
| 003 | AR-BaUEN | ||
| 005 | 20250306084106.0 | ||
| 008 | 190411s2000 xx ||||fo|||| 00| 0 eng|d | ||
| 024 | 7 | |2 scopus |a 2-s2.0-6744271968 | |
| 040 | |a Scopus |b spa |c AR-BaUEN |d AR-BaUEN | ||
| 100 | 1 | |a Van Driel-Gesztelyi, L. | |
| 245 | 1 | 0 | |a Initiation of CMEs: The role of magnetic twist |
| 260 | |b Elsevier Ltd |c 2000 | ||
| 270 | 1 | 0 | |m Van Driel-Gesztelyi, L.; Observatoire de Paris, D.A.S.O.P., F-92195, Meudon, France; email: lidia.vandriel@obspm.fr |
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| 506 | |2 openaire |e Política editorial | ||
| 520 | 3 | |a Recent multiwavelength observations, modelling results and theoretical developments indicate the importance of twisted magnetic configurations in solar active regions (ARs) in the initiation of coronal mass ejections (CMEs). Through multiwavelength analysis of a few representative events we make an attempt to provide constraints for CME models. The two events presented here in detail start with the expansion of sigmoids (S- or inverse S-shaped loops) observed in soft X-rays. Both events (on 25 October 1994 and 14 October 1995) occurred before the launch of the SOHO spacecraft, but indirect evidences (i.e. signatures of an outward propagation traced up to ≈20 solar radii and an associated magnetic cloud) suggest that both of them were related to CMEs. We show evidence that sigmoids are the coronal manifestations of twisted magnetic flux tubes, which start expanding presumably due to a loss of equilibrium. It is noteworthy that the analysed CMEs occurred in a complex (not simply bipolar) magnetic environment and in all cases we found evidences of the interaction (magnetic reconnection) with the surrounding fields. We propose a scenario for sigmoid expansion related CME events and suggest that twisted magnetic configurations are good candidates for being source regions of CMEs. © 2000 Elsevier Science B.V. |l eng | |
| 536 | |a Detalles de la financiación: Centre Hospitalier Régional Universitaire de Montpellier | ||
| 536 | |a Detalles de la financiación: Centre National de la Recherche Scientifique | ||
| 536 | |a Detalles de la financiación: T-026165,, T032846, AKP 97-58 2,2, OTKA T-026165, TP096 | ||
| 536 | |a Detalles de la financiación: Agencia Nacional de Promoción Científica y Tecnológica, A97U01 | ||
| 536 | |a Detalles de la financiación: Conseil National de la Recherche Scientifique, USR B7040 | ||
| 536 | |a Detalles de la financiación: We thank Brigitte Schmieder and David Webb for inviting our paper for presentation at the IUGG 99 GA 4.02 session on “CMEs, eruptions and flares: onsets and relationships” held at Birmingham, England on 22 July 1999. We thank the anonymous referee and David Webb for their thorough comments which greatly helped us to improve the paper. We thank the Yohkoh Team and the MSSL YDAC for the Yohkoh/SXT data. The NSO/Kitt Peak magnetogram used in this paper were produced cooperatively by NSF, NOAO, NASA, GSFC and NOAA/SEL, courtesy Karen L. Harvey. We thank Tom Metcalf for the linear force-free magnetic field extrapolation program package we used on the Hawaii Stokes vector magnetic data. The Unité Scientifique de Nançay (Nançay Radio Observatory) of the Observatoire de Paris is associated to the French Centre National de Recherche Scientifique (CNRS) USR B7040 and acknowledges the financial support of the Région Centre. LvDG was supported by the Hungarian Government grants TP096, OTKA T-026165, T032846 and AKP 97-58 2,2. M.L.F, C.H.M. and P.D. acknowledge financial support from ECOS (France) and ANPCYT (Argentina) through their cooperative science program (A97U01). The work of G.A. is supported by NASA and NRL. | ||
| 593 | |a Observatoire de Paris, D.A.S.O.P., F-92195, Meudon, France | ||
| 593 | |a Konkoly Observatory, Pf. 67, H-1525, Budapest, Hungary | ||
| 593 | |a Radio Astronomy Centre (NCRA), Tata Inst. Fundamental Res., (Ooty), Udhagamandalam, India | ||
| 593 | |a NRL, Code 7670, Washington, DC 20375, United States | ||
| 593 | |a GMU, CSI, 4400 University Dr., Fairfax, VA 22030, United States | ||
| 593 | |a IAFE-CONICET, CC.67, Suc.28, 1428, Buenos Aires, Argentina | ||
| 593 | |a University of Oslo, N-0315, Oslo, Norway | ||
| 593 | |a Osserv. Astron. Palermo g.S. Vaiana, I-90134, Palermo, Italy | ||
| 593 | |a NASA / Goddard SFC, Greenbelt, MD 20771, United States | ||
| 593 | |a USRA, Naval Research Laboratory, Washington, DC 20375, United States | ||
| 690 | 1 | 0 | |a CORONAL MASS EJECTIONS |
| 690 | 1 | 0 | |a MAGNETIC TWIST |
| 700 | 1 | |a Manoharan, P.K. | |
| 700 | 1 | |a Démoulin, Pascal | |
| 700 | 1 | |a Aulanier, G. | |
| 700 | 1 | |a Mandrini, C.H. | |
| 700 | 1 | |a Lopez-Fuentes, M. | |
| 700 | 1 | |a Schmieder, B. | |
| 700 | 1 | |a Orlando, S. | |
| 700 | 1 | |a Thompson, B. | |
| 700 | 1 | |a Plunkett, S. | |
| 773 | 0 | |d Elsevier Ltd, 2000 |g v. 62 |h pp. 1437-1448 |k n. 16 |p J. Atmos. Sol.-Terr. Phys. |x 13646826 |w (AR-BaUEN)CENRE-5432 |t Journal of Atmospheric and Solar-Terrestrial Physics | |
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