Astronomy and Astrophysics – Astronomy
Scientific paper
Jun 1983
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1983mnras.203.1011e&link_type=abstract
Monthly Notices of the Royal Astronomical Society (ISSN 0035-8711), vol. 203, June 1983, p. 1011-1020.
Astronomy and Astrophysics
Astronomy
122
Star Clusters, Stellar Evolution, Stellar Models, Stochastic Processes, B Stars, Mass Distribution, O Stars, Statistical Analysis, Stellar Luminosity, Stellar Mass
Scientific paper
Statistical analyses of observed star formation are employed to develop a stochastic model of star formation in dense cloud cores. It is assumed that the stars form at random, with a distribution following some initial mass distribution. Studies of both the stellar densities in gas-free galactic clusters and the gas densities in star-forming molecular clouds indicate that bound clusters form at an efficiency of at least 10 pct. The stochastic formulation is defined by reasoning that the most abundant stars form first and the least abundant after a delay. The maximum masses of clusters is expressed as a function of the mass of the most massive member, and an estimate is performed of the upper limit of the mass of a bound cluster, i.e., 1000-10,000 solar masses, which agrees with velocity dispersion data. Star formation is expected to continue until a critical luminosity is reached, at which point the cloud core is disrupted and the gas leaves. Formation efficiencies over 50 pct will permit the bound cluster to remain. It is expected that the most massive stars will form in the most massive clouds, and then only after low mass stars have already formed.
No associations
LandOfFree
Quiescent formation of bound galactic clusters does not yet have a rating. At this time, there are no reviews or comments for this scientific paper.
If you have personal experience with Quiescent formation of bound galactic clusters, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and Quiescent formation of bound galactic clusters will most certainly appreciate the feedback.
Profile ID: LFWR-SCP-O-1508393