Star formation in differentially rotating galactic disks: The physics of self-propagation.

Bibcode
1994MNRAS.270...75P
Franco, J.; Tenorio-Tagle, G.; Palous, J.
Bibliographical reference

Monthly Notices of the Royal Astronomical Society, Vol. 270, 75.

Advertised on:
9
1994
Journal
Monthly Notices of the Royal Astronomical Society
Number of authors
3
IAC number of authors
1
Citations
33
Refereed citations
21
Description
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 resultin 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 radia distributions of H i and H2, the numbers of multisupernova remnants and massiv( 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 th( observed galaxies. Key words: stars: formation - supernova remnants - galaxies: ISM - galaxies: stella content - galaxies: structure.
Type
Refereed

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