Chemical Enrichment of the Early Solar System Public Deposited
- Last Modified
- March 20, 2019
- Creator
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Goodson, Matthew
- Affiliation: College of Arts and Sciences, Department of Physics and Astronomy
- Abstract
- Meteorites preserved from the birth of the Solar system over 4.5 billion years ago contain the chemical signature of a nearby contemporaneous stellar explosion in the form of short-lived radioisotopes (SLRs) such as Aluminum-26. Yet results from hydrodynamical models of SLR injection into the pre-Solar cloud or disk encounter a common problem: it is difficult to sufficiently mix the hot, enriched gas into the cold, dense, cloud without disrupting the formation of the Solar system. I first consider the role of numerical methods in limiting the mixing. I implement six turbulence models in the Athena hydrodynamics code. I then explore an alternative mechanism to overcome the mixing barrier: microscopic dust grains. I numerically model the interaction of a supernova remnant containing SLR-rich dust grains with a nearby molecular cloud. The results suggest that SLR transport on dust grains is a viable mechanism to explain Solar system enrichment. Finally, I attempt to constrain the formation timescale of stellar systems such as the Solar system using deuterium fractionation as a "chemical clock". I determine the physical conditions necessary to reach the observed values of deuterium fraction in pre-stellar cores.
- Date of publication
- May 2017
- Keyword
- DOI
- Resource type
- Rights statement
- In Copyright
- Advisor
- Evans, Charles
- Heitsch, Fabian
- Law, Nicholas
- Iliadis, Christian
- Drut, Joaquin
- Degree
- Doctor of Philosophy
- Degree granting institution
- University of North Carolina at Chapel Hill Graduate School
- Graduation year
- 2017
- Language
- Parents:
This work has no parents.
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Goodson_unc_0153D_16856.pdf | 2019-04-09 | Public |
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