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- W2099524096 abstract "The evolution of a superbubble is simulated using a local three-dimensional, non-ideal MHD model, which includes galactic differential rotation, an external gravitational potential, heating via supernova explosions and radiative cooling of the in- terstellar medium (ISM). In our model a superbubble is formed due to the clustering of supernova activity, mimicking an OB association. Supernovae are modelled as instantaneous explo- sions that release 10 51 erg of thermal energy and3M of gas in a small volume. We implement a superbubble with the luminosity 310 37 ergs 1 into an initial ISM, which is taken from our ear- lier calculations modelling the warm and hot phases of the ISM. The simulated ISM has a multi-phase structure with hot, dilute and warm, denser gas coexisting in pressure equilibrium; there is also some cold, dense gas in the form of clouds and filaments arising from supernova compression. The multicomponent gas is in a state of developed turbulence, with r.m.s. velocity 10 and 40kms 1 for the warm and hot gas, respectively. At the devel- oped state of the simulation there is a magnetic field of 1.3 G strength having both uniform and random components. The evolution of a superbubble is rather different from that indicated by models with quasi-uniform ambient medium. The superbubble loses its spherical symmetry at very early stages of expansion. Its break-through from the disc is strongly facilitated by the nonuniformity of its environment. A superbubble which would be confined in the disc according to criteria obtained for a quasi-uniform ISM can break out to the halo." @default.
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- W2099524096 date "1999-10-01" @default.
- W2099524096 modified "2023-09-23" @default.
- W2099524096 title "Evolution of a superbubble in a turbulent, multi-phased and magnetized ISM" @default.
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