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r Process Nucleosynthesis in Neutron Star Mergers with the New Nuclear Reaction Network SkyNet

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Figure

Figure 1.1: Observed abundances in our solar system as a function of mass numberA. The lightest elements were created in the Big Bang and fusion in stars predom-inantly creates alpha elements
Figure 1.2: Computed abundances of 4He, D, 3He, and 7Li (blue lines) as a functionof the baryon-to-photon ratio η
Figure 1.3: Cartoon of the early stages of stellar evolution. The star starts out fusinghydrogen to helium in its core
Figure 1.4: Central density and temperature of a 15 Mthe star evolves, the central density and temperature increase, successively ignitinghydrogen, helium, carbon, oxygen, and silicon burning
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