Nucleation of Iron Dust From Type II Supernovae Public

http://ir.library.oregonstate.edu/concern/undergraduate_thesis_or_projects/wm117q42f

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  • When a star dies in a supernova, its constituent particles are torn apart and a gaseous cloud of atoms remains. These atoms may eventually condense again into large bodies such as planets and stars. There are three main theories as to how this happens: classical, kinetic, and non-local thermodynamic equilibrium (non-LTE). In the classical theory, no nucleation can occur below a critical density and saturation and does not account for much of the nucleation that must occur in the interstellar medium(ISM). The kinetic and non-LTE theories allow for nucleation to occur below the classical critical levels. Most research into this area so far has been focused on the formation of carbon dust. Carbon has a very specific geometry and behaves rather uniquely from a chemical perspective. I was curious as to how a difference in atomic geometry and chemical behavior would affect the formation of dust particles. To investigate this, I am studying the formation of iron dust in supernova remnants. The assumptions that the iron in the supernova remnants exists solely as individual atoms, that the iron atoms are spherical, and that cloud is composed solely of iron atoms all simplified the initial results. Once reasonable results are obtained with these assumptions, they may be removed in order to get a more realistic picture of the formation of iron dust.
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  • description.provenance : Submitted by Lisa Fletcher (chavelal@onid.orst.edu) on 2015-06-08T04:08:04Z No. of bitstreams: 2 license_rdf: 1232 bytes, checksum: bb87e2fb4674c76d0d2e9ed07fbb9c86 (MD5) FletcherLisaM2015.pdf: 625670 bytes, checksum: 737d3841ceeb32ee3bff6568678b72dc (MD5)
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