The magnetic helicity budget of a CME-prolific active region

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Coronal mass ejections (CMEs) are thought to be the way by which the solar corona expels accumulated magnetic helicity which is injected into the corona via several methods. DeVore (2000) suggests that a significant quantity is injected by the action of differential rotation, however Démoulin et al....

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Autor principal: Green, L.M
Otros Autores: López Fuentes, M.C, Mandrini, C.H, Démoulin, Pascal, Van Driel-Gesztelyi, L., Culhane, J.L
Formato: Capítulo de libro
Lenguaje:Inglés
Publicado: 2002
Acceso en línea:Registro en Scopus
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Biblioteca Central Dr. Luis F. Leloir (FCEN) de Universidad de Buenos Aires
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100 1 |a Green, L.M. 
245 1 4 |a The magnetic helicity budget of a CME-prolific active region 
260 |c 2002 
270 1 0 |m Inst. de Astronomia/Fis. del Espacio, IAFE, CC. 67 Suc. 28, 1428 Buenos Aires, Argentina; email: lmg@mssl.ucl.ac.uk 
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506 |2 openaire  |e Política editorial 
520 3 |a Coronal mass ejections (CMEs) are thought to be the way by which the solar corona expels accumulated magnetic helicity which is injected into the corona via several methods. DeVore (2000) suggests that a significant quantity is injected by the action of differential rotation, however Démoulin et al. (2002b), based on the study of a simple bipolar active region, show that this may not be the case. This paper studies the magnetic helicity evolution in an active region (NOAA 8100) in which the main photospheric polarities rotate around each other during five Carrington rotations. As a result of this changing orientation of the bipole, the helicity injection by differential rotation is not a monotonic function of time. Instead, it experiences a maximum and even a change of sign. In this particular active region, both differential rotation and localized shearing motions are actually depleting the coronal helicity instead of building it. During this period of five solar rotations, a high number of CMEs (35 observed, 65 estimated) erupted from the active region and the helicity carried away has been calculated, assuming that each can be modeled by a twisted flux rope. It is found that the helicity injected by differential rotation (≈ -7 × 1042 Mx2) into the active region cannot provide the amount of helicity ejected via CMEs, which is a factor 5 to 46 larger and of the opposite sign. Instead, it is proposed that the ejected helicity is provided by the twist in the sub-photospheric part of the magnetic flux tube forming the active region.  |l eng 
536 |a Detalles de la financiación: A01U04 
536 |a Detalles de la financiación: T-038013, T-032846 
536 |a Detalles de la financiación: Royal Society, F/01/004 
536 |a Detalles de la financiación: L.M.G. is grateful to PPARC for postgraduate student funding. P.D., C.H.M. and M.C.L.F. acknowledge financial support from ECOS (France) and SETCIP (Argentina) through their cooperative science program (A01U04). L.v.D.G. is supported by the Hungarian Government grants OTKA T-032846, T-038013. P.D. and L.v.D.G. acknowledge the Hungarian–French S&T cooperative program. We are grateful to the Royal Society for the award of a European Joint Project grant. C.H.M. thanks the Solar Physics Group at MSSL for their hospitality and for an MSSL Visitor’s Grant. These results were obtained in the framework of the projects OT/98/14 (K.U. Leuven), G.0344.98 (FWO-Vlaanderen), and 14815/00/NL/SFe(IC) (ESA Prodex 6). LVD is supported by Research Fellowship F/01/004 of the K.U. Leuven. The authors thank the MDI, EIT and LASCO consortia and the Yohkoh/SXT team for their data. SOHO is a project of international cooperation between ESA and NASA. Yohkoh is a mission of the Japanese Institute for Space and Astronautical Science. We acknowledge the SURF for providing data for this publication. 
593 |a Inst. de Astronomia/Fis. del Espacio, IAFE, CC. 67 Suc. 28, 1428 Buenos Aires, Argentina 
593 |a Observatoire de Paris, Section Meudon, LESIA (CNRS), F-92195 Meudon Principal Cedex, France 
593 |a Centre for Plasma Astrophysics, K.U. Leuven, Celestijnenlaan 200B, 3001 Heverlee, Belgium 
700 1 |a López Fuentes, M.C. 
700 1 |a Mandrini, C.H. 
700 1 |a Démoulin, Pascal 
700 1 |a Van Driel-Gesztelyi, L. 
700 1 |a Culhane, J.L. 
773 0 |d 2002  |g v. 208  |h pp. 43-68  |k n. 1  |p Sol. Phys.  |x 00380938  |w (AR-BaUEN)CENRE-2238  |t Solar Physics 
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