Mathematics – Probability
Scientific paper
Jul 1985
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985apj...294..523e&link_type=abstract
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 294, July 15, 1985, p. 523-532.
Mathematics
Probability
64
Mass Ratios, Milky Way Galaxy, Molecular Clouds, Star Clusters, Stellar Evolution, Astronomical Models, Hydrogen Clouds, Monte Carlo Method, Stellar Luminosity, Stellar Mass, Stellar Winds
Scientific paper
The formation rate of galactic clusters is estimated to be 2.5±1×10-7kpc-2yr-1 from published tables of cluster positions and ages. This low rate and the observed high space density of low-mass clouds, combined with the relatively high predicted value of the formation probability of a bound cluster per low-mass cloud, suggest either that low-mass clouds typically form stars for over ≡100 free-fall times, or that such clouds avoid forming bound clusters by mechanisms unrelated to internal stellar disruption. Because the formation rate of bound clusters is approximately the same as the formation rate of OB associations, most bound clusters may form in giant molecular clouds, along with associations. In that case, low-mass clouds must strongly avoid forming bound clusters, even though they have enough mass to do so and their star formation efficiencies are probably high enough. Possible reasons for this avoidance are discussed.
Clemens Cathy
Elmegreen Bruce G.
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