Abstract
Astrophysical simulations require knowledge of a wide array of reaction rates. For a number of reasons, many of these reaction rates cannot be measured directly and instead are probed with indirect nuclear reactions. We review the current state of the art regarding the techniques used to extract reaction information that is relevant to describe stars, including their explosions and collisions. We focus on the theoretical developments over the last decade that have had an impact on the connection between the laboratory indirect measurement and the astrophysical desired reaction. This review includes three major probes that have been, and will continue to be, widely used in our community: transfer reactions, breakup reactions, and charge-exchange reactions.
Highlights
Parallel, the progress of multidimensional models for core-collapse supernovae is still in the early stages when it comes to nucleosynthesis [8]
In addition to structure properties such as mass and β-decay rate, crucial nuclear inputs include a variety of reaction cross sections on rare isotopes at a wide range of energies that, depending on the astrophysical conditions, can go from keV to MeV
There has been substantial progress in the reaction theories associated with describing transfer, breakup, and charge-exchange reactions, and it is important that these significant improvements percolate into the nuclear astrophysics world
Summary
One-nucleon transfer reactions at low/intermediate beam energies (5 MeV per nucleon Ebeam 50 MeV per nucleon) are one of the standard experimental tools to probe single-nucleon degrees of freedom in nuclei. The nuclear mechanism for capturing a nucleon in a specific bound state or resonance favors states with high singleparticle content The interplay of these two aspects of nuclear structure determines the way in which the incoming nucleon is absorbed by the nucleus A, and the dominance of one kind of capture over the other will evolve along a given isotopic chain (see, e.g., 18). These two physical mechanisms require the knowledge of different aspects of nuclear structure, and they are addressed with distinct experimental tools. Neutron-transfer reactions with γ -ray coincidences [e.g., (d, pγ ) with rare isotope beams] could inform both processes
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