Abstract
One main characteristic of the ionized and neutral component of the interstellar medium in galaxies is the appearance of shells and bubbles in all sizes up to 1 kpc diameter (Hodge,1974; Heiles, 1979). Between different galaxy types differences in size and radial distribution of these bubbles are observed as a function of galaxy type. The stochastic selfpropagating star formation model is able to simulate such distributions on a global galactic scale.
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Bruhweiler, F., Gull, T.R., Kafatos, M., Sofia, S., 1980, Ap. J. 238, L27
Feitzinger, J.V., Glassgold, A.E., Gerola, H., Seiden, P.E., 1981, Astronomy Astrophys. 98, 371
Heiles, C., 1979, Ap. J. 229, 533
Hodge, P.W., 1974, PASP 86, 845
Seiden, P.E., Schulman, L.S., Feitzinger, J.V., 1982, Ap. J. 253, 91
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© 1983 IAU
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Feitzinger, J.V., Seiden, P.E. (1983). Model Calculations on the Large Scale Distribution of Bubbles in Galaxies. In: Athanassoula, E. (eds) Internal Kinematics and Dynamics of Galaxies. International Astronomical Union/Union Astronomique Internationale, vol 100. Springer, Dordrecht. https://doi.org/10.1007/978-94-009-7075-5_37
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DOI: https://doi.org/10.1007/978-94-009-7075-5_37
Publisher Name: Springer, Dordrecht
Print ISBN: 978-90-277-1547-0
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