osnaDocs: Modeling Solar Cosmic Ray Transport within the Ecliptic Plane

Modeling Solar Cosmic Ray Transport within the Ecliptic Plane

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https://osnadocs.ub.uni-osnabrueck.de/handle/urn:nbn:de:gbv:700-2012040410112

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DC Field	Value	Language
dc.contributor.advisor	Prof. Dr. May-Britt Kallenrode
dc.creator	Lampa, Florian
dc.date.accessioned	2012-04-04T16:09:05Z
dc.date.available	2012-04-04T16:09:05Z
dc.date.issued	2012-04-04T16:09:05Z
dc.identifier.uri	https://osnadocs.ub.uni-osnabrueck.de/handle/urn:nbn:de:gbv:700-2012040410112	-
dc.description.abstract	Since six decades the understanding of interplanetary propagation of solar flare accelerated, energetic charged particles in the inner heliosphere has not yet achieved sufficient closure. The essential mechanisms acting on these charged particles, which perform helical orbits along the large-scale magnetic field lines as probes, have already been identified. However, in particular the impact of the three-dimensional, small-scale magnetic fluctuations on the particles' trajectories has not yet been fully understood. These superimposed disturbances are expected to interact with the charges via resonance principle – leading to both field-aligned scattering and diffusive cross-field displacements of the particles' guiding center. Since numerical solutions and known theoretical formulations have failed to verify the measurements so far, Ruffolo's equation – which is a special formulation of the Fokker-Planck equation – is applied to take account of the current knowledge about field-parallel transport; The partial differential equation is extended to a two-dimensional model within the ecliptic plane by a spatial diffusion term perpendicular to the field. We assume an idealized Archimedean field neither with polarity changes nor large-scale disturbances such as traveling magneto-hydrodynamic shock waves or magnetic clouds. The transport equation is solved numerically by finite differences. For typical ratios of perpendicular to parallel diffusion coefficient as deduced from theory, various fits have been found in good agreement with multi-spacecraft measurements. Some events and the occurrence of observed sudden flux drop-outs suggest that scattering on magnetic field irregularities significantly varies from one flux tube to another. In addition to the already existing, but sparse set of particle observations at different positions, once the current solar minimum has passed by, a new set will be available from the recently launched STEREO satellites.	eng
dc.subject	plasma physics	eng
dc.subject	astrophysics	eng
dc.subject	solar	eng
dc.subject	energetic	eng
dc.subject	particles	eng
dc.subject	cosmic	eng
dc.subject	rays	eng
dc.subject	flare	eng
dc.subject	ecliptic	eng
dc.subject	transport	eng
dc.subject.ddc	530 - Physik
dc.title	Modeling Solar Cosmic Ray Transport within the Ecliptic Plane	eng
dc.title.alternative	Modellierung des Transports solarer energiereicher Teilchen in der Ebene der Ekliptik	ger
dc.type	Dissertation oder Habilitation [doctoralThesis]	-
thesis.location	Osnabrück	-
thesis.institution	Universität	-
thesis.type	Dissertation [thesis.doctoral]	-
thesis.date	2011-05-06	-
dc.contributor.referee	Prof. Dr. Philipp Maass
vCard.ORG	FB4
Appears in Collections:	FB06 - E-Dissertationen

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