TY - JOUR
T1 - The Impact of Nuclear Reaction Rate Uncertainties on the Evolution of Core-collapse Supernova Progenitors
AU - Fields, C. E.
AU - Timmes, Francis
AU - Farmer, R.
AU - Petermann, I.
AU - Wolf, William M.
AU - Couch, S. M.
N1 - Funding Information:
S.M.C. is supported by the U.S. Department of Energy, Office of Science, Office of Nuclear Physics, under Award Numbers DE-SC0015904 and DESC0017955, the Research Corporation for Science Advancement under Scialog Grant 23770, and the Chandra X-ray Observatory under grant TM7-18005X. The simulations presented in this work were performed on the laconia cluster supported by the Institute for Cyber-Enabled Research (ICER) at Michigan State University. This research made extensive use of the SAO/NASA Astrophysics Data System (ADS).
Funding Information:
This project was supported by NSF under the Software Infrastructure for Sustained Innovation (SI2) program grants (ACI-1339581, ACI-1339600, ACI-1339606, ACI-1663684, ACI-1663688, ACI-1663696) and grant PHY-1430152 for the Physics Frontier Center “Joint Institute for Nuclear Astrophysics—Center for the Evolution of the Elements” (JINA-CEE). This project was also supported by NASA under the Theoretical and Computational Astrophysics Networks (TCAN) program grants (NNX14AB53G, NNX14AB55G, NNX12AC72G) and the Astrophysics Theory Program grant 14-ATP14-0007. C.E.F. acknowledges support from a Predoctoral Fellowship administered by the National Academies of Sciences, Engineering, and Medicine on behalf of the Ford Foundation, an Edward J Petry Graduate Fellowship from Michigan State University, and the National Science Foundation Graduate Research Fellowship Program under grant number DGE1424871. S.M.C. is supported by the U.S. Department of Energy, Office of Science, Office of Nuclear Physics, under Award Numbers DE-SC0015904 and DESC0017955, the Research Corporation for Science Advancement under Scialog Grant 23770, and the Chandra X-ray Observatory under grant TM7-18005X. The simulations presented in this work were performed on the laconia cluster supported by the Institute for Cyber-Enabled Research (ICER) at Michigan State University. This research made extensive use of the SAO/NASA Astrophysics Data System (ADS).
Publisher Copyright:
© 2018. The American Astronomical Society. All rights reserved.
PY - 2018/2
Y1 - 2018/2
N2 - We explore properties of core-collapse supernova progenitors with respect to the composite uncertainties in the thermonuclear reaction rates by coupling the probability density functions of the reaction rates provided by the STARLIB reaction rate library with MESA stellar models. We evolve 1000 models of 15 from the pre-main sequence to core O-depletion at solar and subsolar metallicities for a total of 2000 Monte Carlo stellar models. For each stellar model, we independently and simultaneously sample 665 thermonuclear reaction rates and use them in a MESA in situ reaction network that follows 127 isotopes from 1H to 64Zn. With this framework we survey the core mass, burning lifetime, composition, and structural properties at five different evolutionary epochs. At each epoch we measure the probability distribution function of the variations of each property and calculate Spearman rank-order correlation coefficients for each sampled reaction rate to identify which reaction rate has the largest impact on the variations on each property. We find that uncertainties in the reaction rates of , triple-α, , 12C(12C,p)23Na, 12C(16O, p)27Al, 16O(16O,n)31S, 16O(16O, p)31P, and 16O(16O,α)28Si dominate the variations of the properties surveyed. We find that variations induced by uncertainties in nuclear reaction rates grow with each passing phase of evolution, and at core H-, He-depletion they are of comparable magnitude to the variations induced by choices of mass resolution and network resolution. However, at core C-, Ne-, and O-depletion, the reaction rate uncertainties can dominate the variation, causing uncertainty in various properties of the stellar model in the evolution toward iron core-collapse.
AB - We explore properties of core-collapse supernova progenitors with respect to the composite uncertainties in the thermonuclear reaction rates by coupling the probability density functions of the reaction rates provided by the STARLIB reaction rate library with MESA stellar models. We evolve 1000 models of 15 from the pre-main sequence to core O-depletion at solar and subsolar metallicities for a total of 2000 Monte Carlo stellar models. For each stellar model, we independently and simultaneously sample 665 thermonuclear reaction rates and use them in a MESA in situ reaction network that follows 127 isotopes from 1H to 64Zn. With this framework we survey the core mass, burning lifetime, composition, and structural properties at five different evolutionary epochs. At each epoch we measure the probability distribution function of the variations of each property and calculate Spearman rank-order correlation coefficients for each sampled reaction rate to identify which reaction rate has the largest impact on the variations on each property. We find that uncertainties in the reaction rates of , triple-α, , 12C(12C,p)23Na, 12C(16O, p)27Al, 16O(16O,n)31S, 16O(16O, p)31P, and 16O(16O,α)28Si dominate the variations of the properties surveyed. We find that variations induced by uncertainties in nuclear reaction rates grow with each passing phase of evolution, and at core H-, He-depletion they are of comparable magnitude to the variations induced by choices of mass resolution and network resolution. However, at core C-, Ne-, and O-depletion, the reaction rate uncertainties can dominate the variation, causing uncertainty in various properties of the stellar model in the evolution toward iron core-collapse.
KW - stars: abundances
KW - stars: evolution
KW - stars: interiors
KW - supernovae: general
UR - http://www.scopus.com/inward/record.url?scp=85042538610&partnerID=8YFLogxK
UR - http://www.scopus.com/inward/citedby.url?scp=85042538610&partnerID=8YFLogxK
U2 - 10.3847/1538-4365/aaa29b
DO - 10.3847/1538-4365/aaa29b
M3 - Article
AN - SCOPUS:85042538610
SN - 0067-0049
VL - 234
JO - Astrophysical Journal, Supplement Series
JF - Astrophysical Journal, Supplement Series
IS - 2
M1 - 19
ER -