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Stochastic Star Formation and Magnetic Fields

Published online by Cambridge University Press:  19 July 2016

J. V. Feitzinger
Affiliation:
Astronomical Institut, Ruhr University Bochum, Observatory of the City of Bochum, Castroper Str. 67, D-4630 Bochum, F.R.G.
E. Harfst
Affiliation:
Astronomical Institut, Ruhr University Bochum, Observatory of the City of Bochum, Castroper Str. 67, D-4630 Bochum, F.R.G.
J. Spicker
Affiliation:
Astronomical Institut, Ruhr University Bochum, Observatory of the City of Bochum, Castroper Str. 67, D-4630 Bochum, F.R.G.

Extract

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The model of selfpropagating star formation uses local processes (200 pc cell size) in the interstellar medium to simulate the large scale cooperative behaviour of spiral structure in galaxies. The dynamic of the model galaxies is taken into account via the mass distribution and the resulting rotation curve; flat rotation curves are used. The interstellar medium is treated as a multiphase medium with appropriate cooling times and density history. The phases are: molecular gas, cool HI gas, warm intercloud and HII gas and hot coronal fountain gas. A detailed gas reshuffeling between the star forming cells in the plane and outside the galactic plane controls the cell content. Two processes working stochastically are incooperated: the building and the decay of molecular clouds and the star forming events in the molecular clouds.

Type
5. The Polarization, Magnetic Field and Velocity Structure of External Spiral Galaxies
Copyright
Copyright © Kluwer 1990 

References

Feitzinger, J. V., Spicker, J. 1987. in Interstellar Magnetic Fields, Eds.: Beck, R., Gräve, R., p. 171. Springer Verlag, Berlin Neukirch, Th., Feitzinger, J. V., 1988, MN 235, 1343 Google Scholar