Star formation in differentially rotating galactic discs: the physics of self-propagation
Open Access
- 1 September 1994
- journal article
- Published by Oxford University Press (OUP) in Monthly Notices of the Royal Astronomical Society
- Vol. 270 (1) , 75-92
- https://doi.org/10.1093/mnras/270.1.75
Abstract
Large-scale propagating star formation in galaxies is studied as a self-regulatin process. The model connects the energy injection by star formation with the resulting interstellar structures in a differentially rotating disc. The star formation cycl includes the formation of new stars in groups, multisupernova remnants agglomerafin the gas into supershells, formation of clouds and repeated birth of stars. We investigat the evolution of a galaxy dominated by this cycle and conclude that the predicted radial distributions of H I and H2, the numbers of multisupernova remnants and massive cloud complexes, the surface filling factors of shells, the star formation rate (SFR), and the location of the molecular rings are in agreement with the properties of the observed galaxies.Keywords
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