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The galactic scale bipolar outflow from the nucleus of a starburst galaxy is studied. A large wind bubble with the size of a few hundred parsecs at the nuclear region of the starburst galaxy results from the frequent supernova explosions as 0.1 supernovae in a year or more. By two-dimensional hydrodynamical simulation, it is shown that the hot matter heated by supernova explosions interacts with ambient interstellar matter and forms the wind bubble structure, i.e., hot cavity and surrounding cooled shell. The bubble gradually elongates with expansion perpendicularly to the galactic disk. Finally, the shell is broken near the top, and the hot matter in the cavity is collimated and accelerated upwardly. Hot gas goes up to 1-2 kpc above the disk plane. This corresponds to the X-ray emission extending perpendicularly to the galactic disk in M82 and NGC 253. Further, the cooled shell formed near the disk plane seems to correspond to the CO spur extending to the halo region in M82.
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Tomisaka et al. (1988) studied this question.
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