Magnetic clouds seen at different locations in the heliosphere
We analyze two magnetic clouds (MCs) observed in different points of the heliosphere. The main aim of the present study is to provide a link between the different aspects of this phenomenon, starting with information on the origins of the MCs at the Sun and following by the analysis of in-situ obser...
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| Autores principales: | , , , , , , , , , , , |
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| Formato: | Artículo publishedVersion |
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2008
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| Acceso en línea: | http://hdl.handle.net/20.500.12110/paper_09927689_v26_n2_p213_Rodriguez https://repositoriouba.sisbi.uba.ar/gsdl/cgi-bin/library.cgi?a=d&c=artiaex&d=paper_09927689_v26_n2_p213_Rodriguez_oai |
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I28-R145-paper_09927689_v26_n2_p213_Rodriguez_oai2024-08-16 Rodriguez, L. Zhukov, A.N. Dasso, S. Mandrini, C.H. Cremades, H. Cid, C. Cerrato, Y. Saiz, E. Aran, A. Menvielle, M. Poedts, S. Schmieder, B. 2008 We analyze two magnetic clouds (MCs) observed in different points of the heliosphere. The main aim of the present study is to provide a link between the different aspects of this phenomenon, starting with information on the origins of the MCs at the Sun and following by the analysis of in-situ observations at 1 AU and at Ulysses. The candidate source regions were identified in SOHO/EIT and SOHO/MDI observations. They were correlated with H-± images that were obtained from ground-based observatories. Hints on the internal magnetic field configuration of the associated coronal mass ejections are obtained from LASCO C2 images. In interplanetary space, magnetic and plasma moments of the distribution function of plasma species (ACE/Ulysses) were analyzed together with information on the plasma composition, and the results were compared between both spacecraft in order to understand how these structures interact and evolve in their cruise from the Sun to 5 AU. Additionally, estimates of global magnitudes of magnetic fluxes and helicity were obtained from magnetic field models applied to the data in interplanetary space. We have found that these magnetic characteristics were well kept from their solar source, up to 5 AU where Ulysses provided valuable information which, together with that obtained from ACE, can help to reinforce the correct matching of solar events and their interplanetary counterparts. Fil:Dasso, S. Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales; Argentina. Fil:Mandrini, C.H. Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales; Argentina. application/pdf http://hdl.handle.net/20.500.12110/paper_09927689_v26_n2_p213_Rodriguez info:eu-repo/semantics/openAccess http://creativecommons.org/licenses/by/2.5/ar Ann. Geophys. 2008;26(2):213-229 cloud magnetic field plasma solar activity Magnetic clouds seen at different locations in the heliosphere info:eu-repo/semantics/article info:ar-repo/semantics/artículo info:eu-repo/semantics/publishedVersion https://repositoriouba.sisbi.uba.ar/gsdl/cgi-bin/library.cgi?a=d&c=artiaex&d=paper_09927689_v26_n2_p213_Rodriguez_oai |
| institution |
Universidad de Buenos Aires |
| institution_str |
I-28 |
| repository_str |
R-145 |
| collection |
Repositorio Digital de la Universidad de Buenos Aires (UBA) |
| topic |
cloud magnetic field plasma solar activity |
| spellingShingle |
cloud magnetic field plasma solar activity Rodriguez, L. Zhukov, A.N. Dasso, S. Mandrini, C.H. Cremades, H. Cid, C. Cerrato, Y. Saiz, E. Aran, A. Menvielle, M. Poedts, S. Schmieder, B. Magnetic clouds seen at different locations in the heliosphere |
| topic_facet |
cloud magnetic field plasma solar activity |
| description |
We analyze two magnetic clouds (MCs) observed in different points of the heliosphere. The main aim of the present study is to provide a link between the different aspects of this phenomenon, starting with information on the origins of the MCs at the Sun and following by the analysis of in-situ observations at 1 AU and at Ulysses. The candidate source regions were identified in SOHO/EIT and SOHO/MDI observations. They were correlated with H-± images that were obtained from ground-based observatories. Hints on the internal magnetic field configuration of the associated coronal mass ejections are obtained from LASCO C2 images. In interplanetary space, magnetic and plasma moments of the distribution function of plasma species (ACE/Ulysses) were analyzed together with information on the plasma composition, and the results were compared between both spacecraft in order to understand how these structures interact and evolve in their cruise from the Sun to 5 AU. Additionally, estimates of global magnitudes of magnetic fluxes and helicity were obtained from magnetic field models applied to the data in interplanetary space. We have found that these magnetic characteristics were well kept from their solar source, up to 5 AU where Ulysses provided valuable information which, together with that obtained from ACE, can help to reinforce the correct matching of solar events and their interplanetary counterparts. |
| format |
Artículo Artículo publishedVersion |
| author |
Rodriguez, L. Zhukov, A.N. Dasso, S. Mandrini, C.H. Cremades, H. Cid, C. Cerrato, Y. Saiz, E. Aran, A. Menvielle, M. Poedts, S. Schmieder, B. |
| author_facet |
Rodriguez, L. Zhukov, A.N. Dasso, S. Mandrini, C.H. Cremades, H. Cid, C. Cerrato, Y. Saiz, E. Aran, A. Menvielle, M. Poedts, S. Schmieder, B. |
| author_sort |
Rodriguez, L. |
| title |
Magnetic clouds seen at different locations in the heliosphere |
| title_short |
Magnetic clouds seen at different locations in the heliosphere |
| title_full |
Magnetic clouds seen at different locations in the heliosphere |
| title_fullStr |
Magnetic clouds seen at different locations in the heliosphere |
| title_full_unstemmed |
Magnetic clouds seen at different locations in the heliosphere |
| title_sort |
magnetic clouds seen at different locations in the heliosphere |
| publishDate |
2008 |
| url |
http://hdl.handle.net/20.500.12110/paper_09927689_v26_n2_p213_Rodriguez https://repositoriouba.sisbi.uba.ar/gsdl/cgi-bin/library.cgi?a=d&c=artiaex&d=paper_09927689_v26_n2_p213_Rodriguez_oai |
| work_keys_str_mv |
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| _version_ |
1809356917075607552 |