Mathematics – Probability
Scientific paper
Jan 1981
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1981mnras.194..169c&link_type=abstract
Monthly Notices of the Royal Astronomical Society, vol. 194, Jan. 1981, p. 169-176. Research supported by the University of Mai
Mathematics
Probability
12
Disk Galaxies, Galactic Evolution, Shock Waves, Spiral Galaxies, Star Formation, Stochastic Processes, Cosmic Dust, Galactic Structure, Interstellar Gas, Supernova Remnants, Supernovae
Scientific paper
The formation of spiral arms in disk galaxies is generally attributed to the effects of spiral density waves. These relatively small (i.e. 5 per cent) non-axisymmetric perturbations of the interstellar medium cause spiral arms highlighted by O and B type stars to be created. This paper examines another mechanism for spiral arm formation, the stochastic self-propagating star formation (SSPSF) process. The SSPSF process combines the theory that shock waves from supernovae will compress the interstellar medium to create new stars, some of which will be massive enough to also supernova, with a disc galaxy's differential rotation to create spiral arms. The present work extends this process to the case where the probability of star formation from supernova shocks decreases with galactic radius. Where this work and previous investigations overlap (namely the uniform probability case), the agreement is very good, pretty spirals with various numbers of arms are generated.
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