Please use this identifier to cite or link to this item: http://hdl.handle.net/2248/3406
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dc.contributor.authorHasan, S. S-
dc.contributor.authorvan Ballegooijen, A. A-
dc.contributor.authorKalkofen, W-
dc.contributor.authorSteiner, O-
dc.date.accessioned2008-09-06T10:39:51Z-
dc.date.available2008-09-06T10:39:51Z-
dc.date.issued2005-10-
dc.identifier.citationAstrophysical Journal, Vol. 631, No. 1, Part 1, pp. 1270 - 1280en
dc.identifier.issn0004-637X-
dc.identifier.urihttp://hdl.handle.net/2248/3406-
dc.description.abstractThe aim of this work is to identify the physical processes that occur in the network and contribute to its dynamics and heating. We model the network as consisting of individual flux tubes, each with a nonpotential field structure, that are located in intergranular lanes. With a typical horizontal size of about 150 km at the base of the photosphere, they expand upward and merge with their neighbors at a height of about 600 km. Above a height of approximately 1000 km the magnetic field starts to become uniform. Waves are excited in this medium by means of motions at the lower boundary. We focus on transverse driving, which generates both fast and slow waves within a flux tube and acoustic waves at the interface of the tube and the ambient medium. The acoustic waves at the interface are due to compression of the gas on one side of the flux tube and expansion on the other. These longitudinal waves are guided upward along field lines at the two sides of the flux tube, and their amplitude increases with height due to the density stratification. Being acoustic in nature, they produce a compression and significant shock heating of the plasma in the chromospheric part of the flux tube. For impulsive excitation with a time constant of 120 s, we find that a dominant feature of our simulations is the creation of vortical motions that propagate upward. We have identified an efficient mechanism for the generation of acoustic waves at the tube edge, which is a consequence of the sharp interface of the flux concentration. We examine some broad implications of our results.en
dc.language.isoenen
dc.publisherThe American Astronomical Societyen
dc.relation.urihttp://www.journals.uchicago.edu/doi/abs/10.1086/432655en
dc.relation.urihttp://arxiv.org/abs/astro-ph/0503525en
dc.subjectMagnetohydrodynamics: MHDen
dc.subjectSun: Chromosphereen
dc.subjectSun: Magnetic Fieldsen
dc.subjectSun: Oscillationsen
dc.titleDynamics of the Solar Magnetic Network: Two-dimensional MHD Simulationsen
dc.typeArticleen
Appears in Collections:IIAP Publications

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