Causes and consequences of magnetic cloud expansion

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Context. A magnetic cloud (MC) is a magnetic flux rope in the solar wind (SW), which, at 1 AU, is observed ∼2-5 days after its expulsion from the Sun. The associated solar eruption is observed as a coronal mass ejection (CME).Aims. Both the in situ observations of plasma velocity distribution and th...

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Detalles Bibliográficos
Autores principales: Démoulin, P., Dasso, S.
Formato: Artículo publishedVersion
Publicado: 2009
Materias:
interplanetary medium
Sun: coronal mass ejections (CMEs)
Sun: magnetic fields
Boundary pressure
Coronal mass ejection
Cylindrical flux ropes
Expansion rate
Flux ropes
Force free fields
In-situ observations
Magnetic clouds
Magnetic energies
Magnetic flux ropes
Magnetic helicity
Plasma velocity
Radial distributions
Radial expansions
Radial velocity
Self-similar
Solar eruption
Astrophysics
Boundary layer flow
Energy conservation
Expansion
Fluid dynamics
Magnetic fields
Magnetic flux
Magnetic structure
Magnetohydrodynamics
Ordinary differential equations
Pressure gradient
Solar wind
Sun
Velocity
Velocity distribution
Solar energy
Acceso en línea:http://hdl.handle.net/20.500.12110/paper_00046361_v498_n2_p551_Demoulin
https://repositoriouba.sisbi.uba.ar/gsdl/cgi-bin/library.cgi?a=d&c=artiaex&d=paper_00046361_v498_n2_p551_Demoulin_oai
Aporte de:
Repositorio Digital de la Universidad de Buenos Aires (UBA) de Universidad de Buenos Aires

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