Abstract
We discuss recent developments in indirect methods used in nuclear astrophysics to determine the capture cross sections and subsequent rates of various stellar burning processes, when it is difficult to perform the corresponding direct measurements. We discuss in brief, the basic concepts of Asymptotic Normalization Coefficients, the Trojan Horse Method, the Coulomb Dissociation Method, (d,p), and charge-exchange reactions.
Highlights
In astrophysics there is a plethora of interesting questions related to the evolution of the Universe, of processes responsible for energy generation in stars and how the nuclei that are observed on Earth are formed
Asymptotic Normalization Coefficient The Asymptotic Normalization Coefficient (ANC) method is based on the normalization of the tail of the quantum overlap of bound state wave functions of the initial and final nuclei [2, 4]
The capture in such case proceeds through the tail of the nuclear overlap of the initial and final bound state wave functions whose shape is completely determined by the Coulomb force and the amplitude of the tail is given by the ANC
Summary
In astrophysics there is a plethora of interesting questions related to the evolution of the Universe, of processes responsible for energy generation in stars and how the nuclei that are observed on Earth are formed. Asymptotic Normalization Coefficient The Asymptotic Normalization Coefficient (ANC) method is based on the normalization of the tail of the quantum overlap of bound state wave functions of the initial and final nuclei [2, 4]. Direct capture reactions of charged particles usually involve systems with small binding energies and they are mostly peripheral at stellar energies.
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