3D MHD Modeling of the Gaseous Structure of the Galaxy: Setup and Initial Results

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dc.creatorGomez, Gilberto C.
dc.creatorCox, Donald P.
dc.date2002-07-29
dc.date.accessioned2026-07-07T10:31:19Z
dc.date.available2026-07-07T10:31:19Z
dc.descriptionWe show the initial results of our 3D MHD simulations of the flow of the Galactic atmosphere as it responds to a spiral perturbation in the potential. In our standard case, as the gas approaches the arm, there is a downward converging flow that terminates in a complex of shocks just ahead of the midplane density peak. The density maximum slants forward at high z, preceeded by a similarly leaning shock. The latter diverts the flow upward and over the arm, as in a hydraulic jump. Behind the gaseous arm, the flow falls again, generating further secondary shocks as it approaches the lower z material. Structures similar to the high z part of the gaseous arms are found in the interarm region of our two-armed case, while broken arms and low column density bridges are present in the four-armed case. We present three examples of what can be learned from these models.
dc.description33 pages, 17 figures. Accepted for publication in Apj. Better quality images in http://www.journals.uchicago.edu/ApJ/journal/preprints/ApJ55782.preprint.pdf
dc.identifierhttps://arxiv.org/abs/astro-ph/0207634
dc.identifierhttp://arxiv.org/abs/astro-ph/0207634
dc.identifierAstrophys.J.580:235-252,2002
dc.identifierdoi:10.1086/343129
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/178370
dc.subjectAstrophysics
dc.title3D MHD Modeling of the Gaseous Structure of the Galaxy: Setup and Initial Results
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