Are There Different Populations of Flux Ropes in the Solar Wind?
Flux ropes are twisted magnetic structures that can be detected by in-situ measurements in the solar wind. However, different properties of detected flux ropes suggest different types of flux-rope populations. As such, are there different populations of flux ropes? The answer is positive and is the...
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Kluwer Academic Publishers
2014
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| 024 | 7 | |2 scopus |a 2-s2.0-84897570577 | |
| 040 | |a Scopus |b spa |c AR-BaUEN |d AR-BaUEN | ||
| 100 | 1 | |a Janvier, M. | |
| 245 | 1 | 4 | |a Are There Different Populations of Flux Ropes in the Solar Wind? |
| 260 | |b Kluwer Academic Publishers |c 2014 | ||
| 270 | 1 | 0 | |m Janvier, M.; Department of Mathematics, University of Dundee, Dundee, DD1 4HN Scotland, United Kingdom; email: mjanvier@maths.dundee.ac.uk |
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| 506 | |2 openaire |e Política editorial | ||
| 520 | 3 | |a Flux ropes are twisted magnetic structures that can be detected by in-situ measurements in the solar wind. However, different properties of detected flux ropes suggest different types of flux-rope populations. As such, are there different populations of flux ropes? The answer is positive and is the result of the analysis of four lists of flux ropes, including magnetic clouds (MCs), observed at 1 AU. The in-situ data for the four lists were fitted with the same cylindrical force-free field model, which provides an estimate of the local flux-rope parameters such as its radius and orientation. Since the flux-rope distributions have a broad dynamic range, we went beyond a simple histogram analysis by developing a partition technique that uniformly distributes the statistical fluctuations across the radius range. By doing so, we found that small flux ropes with radius R<0.1 AU have a steep power-law distribution in contrast to the larger flux ropes (identified as MCs), which have a Gaussian-like distribution. Next, from four CME catalogs, we estimated the expected flux-rope frequency per year at 1 AU. We found that the predicted numbers are similar to the frequencies of MCs observed in-situ. However, we also found that small flux ropes are at least ten times too abundant to correspond to CMEs, even to narrow ones. Investigating the different possible scenarios for the origin of these small flux ropes, we conclude that these twisted structures can be formed by blowout jets in the low corona or in coronal streamers. © 2014 Springer Science+Business Media Dordrecht. |l eng | |
| 536 | |a Detalles de la financiación: Abdus Salam International Centre for Theoretical Physics | ||
| 536 | |a Detalles de la financiación: UBACyT 20020120100220 | ||
| 536 | |a Detalles de la financiación: Abdus Salam International Centre for Theoretical Physics | ||
| 536 | |a Detalles de la financiación: AXA Research Fund | ||
| 536 | |a Detalles de la financiación: Acknowledgements The present work was partially funded by a contract from the AXA Research Fund (MJ) and also supported by the Argentinean grant UBACyT 20020120100220 (SD) and by a one-month invitation of SD by the Paris Observatory. SD is member of the Carrera del Investigador Científico, CONICET. SD acknowledges support from the Abdus Salam International Centre for Theoretical Physics (ICTP), as provided in the framework of his regular associateship. | ||
| 593 | |a Department of Mathematics, University of Dundee, Dundee, DD1 4HN Scotland, United Kingdom | ||
| 593 | |a Observatoire de Paris, LESIA, UMR 8109 (CNRS), 92195 Meudon Principal Cedex, France | ||
| 593 | |a Instituto de Astronomía y Física del Espacio, UBA-CONICET, CC. 67, Suc. 28, 1428 Buenos Aires, Argentina | ||
| 593 | |a Departamento de Física, Facultad de Ciencias Exactas y Naturales, UBA, Buenos Aires, Argentina | ||
| 690 | 1 | 0 | |a CORONAL MASS EJECTIONS |
| 690 | 1 | 0 | |a CORONAL MASS EJECTIONS, INTERPLANETARY |
| 690 | 1 | 0 | |a MAGNETIC FIELDS, INTERPLANETARY |
| 690 | 1 | 0 | |a SOLAR WIND |
| 700 | 1 | |a Démoulin, Pascal | |
| 700 | 1 | |a Dasso, Sergio Ricardo | |
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