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Selfpropagating Stochastic Star Formation and Spiral Structure

Published online by Cambridge University Press:  04 August 2017

J. V. Feitzinger  and
P. E. Seiden
J. V. Feitzinger
Affiliation:
Astronomical Institut, Ruhr-University, Bochum, FRG
P. E. Seiden
Affiliation:
IBM Watson Research Laboratory, Yorktown Heights, NY 10598, USA

Extract

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Spiral structure in galaxies can arise from both dynamic and non dynamic phenomena: spiral density waves and stochastic selfpropagating star formation. The relative importance of these effects is still not known. Deficiences of the original selfpropagating star formation model (where only stars are taken into account) are overcome by explicitly considering the stars embedded in and interacting with a two-component gas (Seiden and Gerola, 1979; Seiden, Schulman and Feitzinger, 1982; Seiden and Gerola, 1982). The two-component gas is essential because it is the means by which we get feedback in the interaction between stars and gas. The coupling between stars and gas regulates and stabilizes star formation in a galaxy. Under proper conditions this model can give good grand design spirals (Fig. 1).

Type
II. Spiral Structure
Information
Symposium - International Astronomical Union , Volume 100: Internal Kinematics and Dynamics of Galaxies , 1983 , pp. 141 - 142
Copyright
Copyright © Reidel 1983 

References

References:

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