Bulletin of the American Physical Society
5th Joint Meeting of the APS Division of Nuclear Physics and the Physical Society of Japan
Volume 63, Number 12
Tuesday–Saturday, October 23–27, 2018; Waikoloa, Hawaii
Session HA: Conference Experience for Undergraduates Poster Session (2:00pm - 3:45pm)
2:00 PM,
Friday, October 26, 2018
Hilton
Room: Grand Promenade
Abstract ID: BAPS.2018.HAW.HA.48
Abstract: HA.00048 : Effects of Input Nuclear Physics on Core Collapse Supernova Simulations
Presenter:
Brandon Barker
(Univ of Tennessee, Knoxville)
Authors:
Brandon Barker
(Univ of Tennessee, Knoxville)
Theo Cooper
(Johns Hopkins)
Michael Pajkos
(Michigan State University)
Jennifer Ranta
(Michigan State University)
MacKenzie Warren
(Michigan State University)
Sean Couch
(Michigan State University)
In the proto-neutron star formed during a core collapse supernova (CCSN), densities can reach several times nuclear density. Due to uncertainties in nuclear physics, there are several different physical models for the equation of state (EOS) at the densities present in the CCSN environment. The outcomes of CCSN simulations can depend sensitively on the EOS. 1D CCSN simulations are key in predictions of the outcome of stellar evolution, neutron star mass distribution, nucleosynthesis, and ultimately, galactic evolution. However, uncertainties in nuclear physics causes changes in these results: simulations using different EOS tables can lead to entirely different predictions. We explore the sensitivity of CCSNe to variations in input nuclear physics. Using 10 different EOS models, we ran 1D CCSN simulations with progenitor masses ranging from 9 to 120 solar masses using a new model for driving 1D explosions that includes the crucial effects of turbulence and convection. A quantitative understanding of how different EOS tables affect the outcome of core collapse is crucial to our ability to make predictions.
To cite this abstract, use the following reference: http://meetings.aps.org/link/BAPS.2018.HAW.HA.48
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