Dynamical evolution of magnetic flux ropes in the solar wind

The conservation of magnetic flux in systems of very low dissipation, as the interplanetary medium, is used to analyze magnetic clouds in significant expansion. In particular, we analyze the fast and huge event observed at one astronomical unit in the solar wind on Nov. 9-10, 2004. We compare magnet...

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Autores principales:	Nakwacki, Maria Soledad, Dasso, Sergio Ricardo, Mandrini, Cristina Hemilse
Publicado:	2008
Materias:	Coronal mass ejections Disturbances Interplanetary Magnetic fields Magnetic reconnection Observational signatures Solar wind astronomy coronal mass ejection geomagnetic field numerical model observational method solar wind spatial variation temporal evolution
Acceso en línea:	https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_00167169_v47_n3_p295_Nakwacki http://hdl.handle.net/20.500.12110/paper_00167169_v47_n3_p295_Nakwacki
Aporte de:	Biblioteca Digital - Facultad de Ciencias Exactas y Naturales (UBA) de Universidad de Buenos Aires

id	paper:paper_00167169_v47_n3_p295_Nakwacki
record_format	dspace
spelling	paper:paper_00167169_v47_n3_p295_Nakwacki2023-06-08T14:38:48Z Dynamical evolution of magnetic flux ropes in the solar wind Nakwacki, Maria Soledad Dasso, Sergio Ricardo Mandrini, Cristina Hemilse Coronal mass ejections Disturbances Interplanetary Magnetic fields Magnetic reconnection Observational signatures Solar wind astronomy coronal mass ejection geomagnetic field numerical model observational method solar wind spatial variation temporal evolution The conservation of magnetic flux in systems of very low dissipation, as the interplanetary medium, is used to analyze magnetic clouds in significant expansion. In particular, we analyze the fast and huge event observed at one astronomical unit in the solar wind on Nov. 9-10, 2004. We compare magnetic and velocity observations to two self-similar and free expansion models that allow us to correct the mixing spatial-variation/time-evolution observed in situ by the spacecrafts. As magnetic clouds are astrophysical objects that transport a very important amount of magnetic flux and helicity from the Sun to the interplanetary medium, we compare the values of these global quantities obtained using the present models with those values coming from the commonly used static Lundquist's model. Fil:Nakwacki, M.S. Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales; Argentina. 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. 2008 https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_00167169_v47_n3_p295_Nakwacki http://hdl.handle.net/20.500.12110/paper_00167169_v47_n3_p295_Nakwacki
institution	Universidad de Buenos Aires
institution_str	I-28
repository_str	R-134
collection	Biblioteca Digital - Facultad de Ciencias Exactas y Naturales (UBA)
topic	Coronal mass ejections Disturbances Interplanetary Magnetic fields Magnetic reconnection Observational signatures Solar wind astronomy coronal mass ejection geomagnetic field numerical model observational method solar wind spatial variation temporal evolution
spellingShingle	Coronal mass ejections Disturbances Interplanetary Magnetic fields Magnetic reconnection Observational signatures Solar wind astronomy coronal mass ejection geomagnetic field numerical model observational method solar wind spatial variation temporal evolution Nakwacki, Maria Soledad Dasso, Sergio Ricardo Mandrini, Cristina Hemilse Dynamical evolution of magnetic flux ropes in the solar wind
topic_facet	Coronal mass ejections Disturbances Interplanetary Magnetic fields Magnetic reconnection Observational signatures Solar wind astronomy coronal mass ejection geomagnetic field numerical model observational method solar wind spatial variation temporal evolution
description	The conservation of magnetic flux in systems of very low dissipation, as the interplanetary medium, is used to analyze magnetic clouds in significant expansion. In particular, we analyze the fast and huge event observed at one astronomical unit in the solar wind on Nov. 9-10, 2004. We compare magnetic and velocity observations to two self-similar and free expansion models that allow us to correct the mixing spatial-variation/time-evolution observed in situ by the spacecrafts. As magnetic clouds are astrophysical objects that transport a very important amount of magnetic flux and helicity from the Sun to the interplanetary medium, we compare the values of these global quantities obtained using the present models with those values coming from the commonly used static Lundquist's model.
author	Nakwacki, Maria Soledad Dasso, Sergio Ricardo Mandrini, Cristina Hemilse
author_facet	Nakwacki, Maria Soledad Dasso, Sergio Ricardo Mandrini, Cristina Hemilse
author_sort	Nakwacki, Maria Soledad
title	Dynamical evolution of magnetic flux ropes in the solar wind
title_short	Dynamical evolution of magnetic flux ropes in the solar wind
title_full	Dynamical evolution of magnetic flux ropes in the solar wind
title_fullStr	Dynamical evolution of magnetic flux ropes in the solar wind
title_full_unstemmed	Dynamical evolution of magnetic flux ropes in the solar wind
title_sort	dynamical evolution of magnetic flux ropes in the solar wind
publishDate	2008
url	https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_00167169_v47_n3_p295_Nakwacki http://hdl.handle.net/20.500.12110/paper_00167169_v47_n3_p295_Nakwacki
work_keys_str_mv	AT nakwackimariasoledad dynamicalevolutionofmagneticfluxropesinthesolarwind AT dassosergioricardo dynamicalevolutionofmagneticfluxropesinthesolarwind AT mandrinicristinahemilse dynamicalevolutionofmagneticfluxropesinthesolarwind
_version_	1768541688078270464

Dynamical evolution of magnetic flux ropes in the solar wind

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