Numerical simulation of large-scale magnetic-field evolution in spiral galaxies

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dc.creatorOtmianowska-Mazur, K.
dc.creatorChiba, M.
dc.date1995-04-02
dc.date.accessioned2026-07-07T02:19:43Z
dc.date.available2026-07-07T02:19:43Z
dc.descriptionThe evolution of large-scale magnetic fields in disk galaxies is investigated numerically. The gasdynamical simulations in a disk perturbed by spiral or bar potential are incorporated into the kinematic calculations of induction equations to elucidate the effects of non-axisymmetric disk structure on magnetic fields. The effects of interstellar turbulence are given as the turbulent diffusion of magnetic fields. The usually adopted dynamo mechanism of alpha-effect is not considered in our computations, because it is not obvious about the actual existence of the effect in a galaxy. Our principal concern is to clear how observationally and theoretically well-established gas flow affects the magnetic-field structure and evolution, without putting a lot of artificial parameters in the model. We have found that the density-wave streaming motion of gas has a significant influence on the distribution of magnetic fields: the lines of force are well aligned with spiral arms due to the compressional and additional shearing flow of gas in these regions.
dc.description14 pages, latex documentstyle {l-aa}
dc.identifierhttps://arxiv.org/abs/astro-ph/9503122
dc.identifierhttp://arxiv.org/abs/astro-ph/9503122
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/9975
dc.subjectAstrophysics
dc.titleNumerical simulation of large-scale magnetic-field evolution in spiral galaxies
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