Other
Scientific paper
Sep 1987
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987mnras.228..229m&link_type=abstract
Monthly Notices of the Royal Astronomical Society (ISSN 0035-8711), vol. 228, Sept. 1, 1987, p. 229-242.
Other
Density Distribution, Dynamic Models, Galactic Evolution, Perturbation Theory, Shock Waves, Supernovae, Astronomical Models, Jeans Theory
Scientific paper
The fate of spherically symmetric, homogeneous density perturbations passed by shock waves from early generations of supernovae is investigated. It is shown that a shock can only influence pregalactic perturbations if the explosion is rather large, or if the initial density contrast is fairly low. For isothermal external or internal shocks perturbation growth may be triggered by the shock. In most other cases, perturbations under influence will be heated to Jeans stability. For the most intense shocks the perturbations will subsequently evaporate. Otherwise the gas cools radiatively (in which case Jeans instability may again be reached) or by Compton cooling (in which case the perturbations usually remain stable). Results are primarily given for an Omega = 1 Universe without nonbaryonic matter, but deviations from this are discussed as well. The study is of relevance to most scenarios of galaxy formation, since supernovae may serve as a feedback mechanism in many contexts. In particular, the investigation has a direct bearing on the explosive scenario and on scenarios relying on bias.
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