Bayesian Estimation Of Thermonuclear Reaction Rates

Iliadis, C.; Anderson, K. S.; Coc, A.; Timmes, F. X.; Starrfield, S.

doi:10.3847/0004-637x/831/1/107

Title: Bayesian Estimation Of Thermonuclear Reaction Rates

Journal Article · Mon Oct 31 00:00:00 EDT 2016 · The Astrophysical Journal (Online)

DOI:https://doi.org/10.3847/0004-637x/831/1/107· OSTI ID:1537160

Iliadis, C. ^[1]; Anderson, K. S. ^[2]; Coc, A. ^[3]; Timmes, F. X. ^[4]; Starrfield, S. ^[5]

Univ. of North Carolina, Chapel Hill, NC (United States). Dept. of Physics & Astronomy; RTI International, Research Triangle Park, NC (United States)
Univ. of North Carolina, Chapel Hill, NC (United States). Dept. of Physics & Astronomy
Centre National de la Recherche Scientifique (CNRS), Orsay (France). Inst. National de Physique Nucleaire et de Physique des Particules (IN2P3), Centre de Sciences Nucleaires et de Sciences de la Matiere (CSNSM)
Arizona State Univ., Tempe, AZ (United States). School of Earth and Space Exploration; Joint Inst. for Nuclear Astrophysics (JINA), East Lansing, MI (United States)
Arizona State Univ., Tempe, AZ (United States). School of Earth and Space Exploration

The problem of estimating non-resonant astrophysical S-factors and thermonuclear reaction rates, based on measured nuclear cross sections, is of major interest for nuclear energy generation, neutrino physics, and element synthesis. Many different methods have been applied to this problem in the past, almost all of them based on traditional statistics. Bayesian methods, on the other hand, are now in widespread use in the physical sciences. In astronomy, for example, Bayesian statistics is applied to the observation of extrasolar planets, gravitational waves, and Type Ia supernovae. However, nuclear physics, in particular, has been slow to adopt Bayesian methods. We present astrophysical S-factors and reaction rates based on Bayesian statistics. We develop a framework that incorporates robust parameter estimation, systematic effects, and non-Gaussian uncertainties in a consistent manner. The method is applied to the reactions d(p,$$γ$$)³He, ³He(³He,2p)⁴He, and ³He(α,$$γ$$)⁷Be, important for deuterium burning, solar neutrinos, and Big Bang nucleosynthesis.

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Research Organization:: University of North Carolina, Chapel Hill, NC (United States); Duke Univ., Durham, NC (United States). Triangle Universities Nuclear Laboratory

Sponsoring Organization:: USDOE Office of Science (SC), Nuclear Physics (NP)

Grant/Contract Number:: FG02-97ER41041; FG02-97ER41033

OSTI ID:: 1537160

Alternate ID(s):: OSTI ID: 1660975; OSTI ID: 1660977

Journal Information:: The Astrophysical Journal (Online), Vol. 831, Issue 1; ISSN 1538-4357

Publisher:: Institute of Physics (IOP)Copyright Statement

Country of Publication:: United States

Language:: English

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Cited by: 34 works

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