Statistical methods for thermonuclear reaction rates and nucleosynthesis simulations
Abstract
Rigorous statistical methods for estimating thermonuclear reaction rates and nucleosynthesis are becoming increasingly established in nuclear astrophysics. The main challenge being faced is that experimental reaction rates are highly complex quantities derived from a multitude of different measured nuclear parameters (e.g., astrophysical Sfactors, resonance energies and strengths, particle and γray partial widths). We discuss the application of the Monte Carlo method to two distinct, but related, questions. First, given a set of measured nuclear parameters, how can one best estimate the resulting thermonuclear reaction rates and associated uncertainties? Second, given a set of appropriate reaction rates, how can one best estimate the abundances from nucleosynthesis (i.e., reaction network) calculations? The techniques described here provide probability density functions that can be used to derive statistically meaningful reaction rates and final abundances for any desired coverage probability. Examples are given for applications to sprocess neutron sources, corecollapse supernovae, classical novae, and Big Bang nucleosynthesis.
 Publication:

Journal of Physics G Nuclear Physics
 Pub Date:
 March 2015
 DOI:
 10.1088/09543899/42/3/034007
 arXiv:
 arXiv:1409.5541
 Bibcode:
 2015JPhG...42c4007I
 Keywords:

 Nuclear Experiment;
 Astrophysics  Solar and Stellar Astrophysics
 EPrint:
 Accepted for publication in J. Phys. G Focus issue "Enhancing the interaction between nuclear experiment and theory through information and statistics"