Please use this identifier to cite or link to this item: http://hdl.handle.net/2248/4960
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dc.contributor.authorHasan, S. S-
dc.contributor.authorVigeesh, G-
dc.contributor.authorvan Ballegooijen, A. A-
dc.date.accessioned2010-01-02T16:31:14Z-
dc.date.available2010-01-02T16:31:14Z-
dc.date.issued2006-
dc.identifier.citationVolker Bothmer; Ahmed Abdel Hady. eds., Solar Activity and its Magnetic Origin, Proceedings of the 233rd Symposium of the International Astronomical Union held in Cairo, Egypt, March 31 - April 4, 2006, pp. 116 - 117en
dc.identifier.isbn0-521-86342-0-
dc.identifier.urihttp://hdl.handle.net/2248/4960-
dc.descriptionRestricted Access-
dc.description.abstractHasan et al. (2005) have recently presented 2-D dynamical calculations on wave propagation in in the magnetic network of the Sun. The latter is idealized as consisting of non-potential flux tubes in the quiet solar chromosphere. It is of interest to understand how the nature of wave propagation is influenced by the choice of initial equilibrium configuration of the magnetic field. We examine this by comparing the earlier calculations with those when the network is modelled as a potential structure. Our calculations demonstrate that the nature of the wave propagation is significantly different, particularly the transport of energy which for the potential case, occurs more isotropically than for the non-potential configuration.en
dc.language.isoenen
dc.publisherCambridge University Pressen
dc.relation.ispartofseriesInternational Astronomical Union Symposium; No. 233-
dc.relation.urihttp://dx.doi.org/10.1017/S174392130600161Xen
dc.subjectSun: Magnetic Fields - Magnetohydrodynamics (MHD)en
dc.subjectSun: Photosphere - Oscillationsen
dc.titleWave propagation in the magnetic network on the Sunen
dc.typeArticleen
Appears in Collections:IIAP Publications

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