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Truran, James W. Brown, James Howard 2011-05-12T15:14:06Z 2011-05-12T15:14:06Z 10000-01-01 1991 This thesis describes a model of globular cluster formation which allows the self contamination of the cluster by an earlier generation of massive stars. It is first shown that such self-contamination naturally produces an [Fe/H] in the range from -2.5 to -1.0, precisely the same range observed in the metal poor (halo) globular clusters; this also seems to require that the disk clusters started with a substantial initial metallicity. To minimize the problem of creating homogeneous globular clusters, the second (currently observed) generation of stars is assumed to form in the expanding supershell around the first generation stars. Both numerical and analytic models are used to address this problem. The most important result of this investigation was that the late evolution of the supershell is the most important, and that this phase of the evolution is dominated by the external medium in which the cloud is embedded. This result and the requirement that only the most tightly bound systems may become globular clusters lead to the conclusion that a globular cluster with the mass and binding energy typically observed can be formed at star formation efficiencies as low as 10-20%. Furthermore, self contamination requires that the typical [Fe/H] of a bound system be about -1.6, independent of the free parameters of the model, allowing the clusters and field stars to form with different metallicity distributions in spite of their forming at the same time. Since the formation of globular clusters in this model is tied to the external pressure, the halo globular cluster masses and distribution can be used as probes of the early galactic structure. In particular, this model requires an increase in the typical globular cluster mass as one moves out from the galactic center; the masses of the halo clusters are examined, and they show considerable evidence for such a gradient. Based on a pressure distribution derived from this data, the effect of the galactic tidal field on the model is also investigated using an N-body simulation. Submitted by Carolyn Mead (cmead2@illinois.edu) on 2011-05-12T15:14:06Z No. of bitstreams: 1 1991_brown.pdf: 3130508 bytes, checksum: 115d8da058e275c6567be318f6de59c8 (MD5) Made available in DSpace on 2011-05-12T15:14:06Z (GMT). No. of bitstreams: 1 1991_brown.pdf: 3130508 bytes, checksum: 115d8da058e275c6567be318f6de59c8 (MD5) Previous issue date: 1991 Item marked as restricted to the 'UIUC Users [automated]' Group (id=2) by Carolyn Mead (cmead2@illinois.edu) on 2011-05-12T15:14:06Z Item is restricted indefinitely. Restriction data tranferred 2014-07-01T11:12:51-05:00 Original Data Group with Access UIUC Users [automated] Release Date: none Reason: Thesis Thesis U of I Only 3476417 http://hdl.handle.net/2142/23872 en 1991 James Howard Brown globular cluster formation self contamination model globular star clusters A self contamination model for the formation of globular star clusters Dissertation / Thesis text Physics Physics University of Illinois at Urbana-Champaign Dissertation Ph.D.