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- W2951629053 abstract "We carried out 1.25 pc resolution MHD simulations of the ISM -- including the large scale galactic fountain -- by fully tracking the time-dependent evolution of the magnetic field and the formation of shock compressed regions in a supernova-driven ISM. The simulations show that large scale gas streams emerge, driven by SN explosions, which are responsible for the formation and destruction of shocked compressed layers with lifetimes up to some 15 Myr. The Tleq 10^{3} K gas is distributed in filaments which tend to show a preferred orientation due to the anisotropy of the flow induced by the galactic magnetic field. The simulations also show that the magnetic field has a high variability, it is largely uncorrelated with the density and it is driven by inertial motions. The latter is consistent with the fact that ram pressure dominates the flow for 10^{2}<Tleq 10^{6} K. For T> 10^{6} K thermal pressure dominates, while for Tleq 10^{2} K (stable branch) magnetic pressure takes over." @default.
- W2951629053 created "2019-06-27" @default.
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- W2951629053 date "2003-11-17" @default.
- W2951629053 modified "2023-09-27" @default.
- W2951629053 title "Does the interstellar magnetic field follow the Chandrasekhar-Fermi law?" @default.
- W2951629053 doi "https://doi.org/10.48550/arxiv.astro-ph/0311394" @default.
- W2951629053 hasPublicationYear "2003" @default.
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