Using the evolution of coronal dimming regions to probe the global magnetic field topology : "Uuunidentical twi"ns: A new interpretation of the 12 May 1997 event
We demonstrate that study of the evolving magnetic nature of coronal dimming regions can be used to probe the large-scale magnetic structure involved in the eruption of a coronal mass ejection (CME). We analyse the intensity evolution of coronal dimming regions using 195 Å data from the Extreme ultr...
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2006
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| LEADER | 09866caa a22010697a 4500 | ||
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| 001 | PAPER-6966 | ||
| 003 | AR-BaUEN | ||
| 005 | 20250618100248.0 | ||
| 008 | 190411s2006 xx ||||fo|||| 00| 0 eng|d | ||
| 024 | 7 | |2 scopus |a 2-s2.0-33751098557 | |
| 040 | |a Scopus |b spa |c AR-BaUEN |d AR-BaUEN | ||
| 100 | 1 | |a Attrill, G. | |
| 245 | 1 | 0 | |a Using the evolution of coronal dimming regions to probe the global magnetic field topology : "Uuunidentical twi"ns: A new interpretation of the 12 May 1997 event |
| 260 | |c 2006 | ||
| 270 | 1 | 0 | |m Attrill, G.; University College London, Mullard Space Science Laboratory, Dorking, Surrey, RH5 6NT, United Kingdom; email: gdra@mssl.ucl.ac.uk |
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| 506 | |2 openaire |e Política editorial | ||
| 520 | 3 | |a We demonstrate that study of the evolving magnetic nature of coronal dimming regions can be used to probe the large-scale magnetic structure involved in the eruption of a coronal mass ejection (CME). We analyse the intensity evolution of coronal dimming regions using 195 Å data from the Extreme ultraviolet Imaging Telescope (EIT) on board the Solar and Heliospheric Observatory (SOHO). We measure the magnetic flux, using data from the SOHO/Michelson Doppler Imager (MDI), in the regions that seem most likely to be related to plasma removal. Then, we compare these magnetic flux measurements to the flux in the associated magnetic cloud (MC). Here, we present our analysis of the well-studied event on 12 May 1997 that took place just after solar minimum in a simple magnetic configuration. We present a synthesis of results already published and propose that driven "interchange reconnection" between the expanding CME structure with ''open'' field lines of the northern coronal hole region led to the asymmetric temporal and spatial evolution of the two main dimming regions, associated with this event. As a result of this reconnection process, we find the southern-most dimming region to be the principal foot-point of the MC. The magnetic flux from this dimming region and that of the MC are found to be in close agreement within the same order of magnitude, 10 21 Mx. © Springer Science + Business Media, Inc. 2006. |l eng | |
| 536 | |a Detalles de la financiación: Philips | ||
| 536 | |a Detalles de la financiación: UBACyT X329, PIP 6220 | ||
| 536 | |a Detalles de la financiación: Agencia Nacional de Promoción Científica y Tecnológica | ||
| 536 | |a Detalles de la financiación: Leverhulme Trust | ||
| 536 | |a Detalles de la financiación: National Natural Science Foundation of China, 10233050 | ||
| 536 | |a Detalles de la financiación: Consejo Nacional de Investigaciones Científicas y Técnicas, PICTs 03-12187, 03-14163 | ||
| 536 | |a Detalles de la financiación: We thank the anonymous referee for helpful comments which greatly improved and clarified this work. SOHO is a project of international cooperation between ESA and NASA. The LASCO CME catalogue is generated and maintained at the CDAW Data Center by NASA and The Catholic University of America in cooperation with the Naval Research Laboratory. This research has made use of NASA’s Space Physics Data Facility (SPDF). G.D.R. Attrill is grateful to PPARC for support. M.S.N. is a fellow of CONICET. L.K.H. acknowledges the Leverhulme Trust for the award of a Philip Leverhulme prize. L.v.D.G. acknowledges the Hungarian government grant OTKA 048961. This work was partially supported by the Argentinean grants UBACyT X329, PIP 6220 (CONICET) and PICTs 03-12187 and 03-14163 (ANPCyT). S.D. and C.H.M. are members of the Carrera del Inves-tigador Científico. J.W. acknowledges support from the National Natural Science Foundation of China under the grant 10233050. | ||
| 593 | |a University College London, Mullard Space Science Laboratory, Dorking, Surrey, RH5 6NT, United Kingdom | ||
| 593 | |a Instituto de Astronomía y Física del Espacio, CONICET-UBA, CC. 67, Suc. 28, 1428 Buenos Aires, Argentina | ||
| 593 | |a Observatoire de Paris, LESIA, FRE 2461 (CNRS), F-92195 Meudon Principal Cedex, France | ||
| 593 | |a Konkoly Observatory, Hungarian Academy of Sciences, Budapest, Hungary | ||
| 593 | |a Departamento de Física, Facultad de Ciencias Exactas y Naturales, Universidad de Buenos Aires, 1428 Buenos Aires, Argentina | ||
| 593 | |a National Astronomical Observatory, Chinese Academy of Sciences, Beijing, China | ||
| 700 | 1 | |a Nakwacki, M.S. | |
| 700 | 1 | |a Harra, L.K. | |
| 700 | 1 | |a Van Driel-Gesztelyi, L. | |
| 700 | 1 | |a Mandrini, Cristina Hemilse | |
| 700 | 1 | |a Dasso, Sergio Ricardo | |
| 700 | 1 | |a Wang, J. | |
| 773 | 0 | |d 2006 |g v. 238 |h pp. 117-139 |k n. 1 |p Sol. Phys. |x 00380938 |w (AR-BaUEN)CENRE-2238 |t Solar Physics | |
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| 856 | 4 | 0 | |u https://hdl.handle.net/20.500.12110/paper_00380938_v238_n1_p117_Attrill |y Handle |
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