This book presents different models used in nuclear astrophysics to derive charged-particle induced cross sections and reaction rates. It focuses on reactions between light elements, such as those involved in the CNO cycle or in He burning. First, a general overview of the main reactions required for stellar evolution is presented. A discussion of the different types of reactions (transfer and capture reactions) is illustrated by some examples. Differences between resonant and non-resonant processes are pointed out. The book starts from general properties of scattering theory and presents general formulas for capture and transfer cross sections. Then, it develops more specifically the potential and R-matrix models, often used in the literature, and applies them to some typical reactions. The use of spectroscopic factors, widespread in nuclear astrophysics, and more generally in low-energy nuclear physics, is discussed. Finally the book considers the calculation of reaction rates. For non-resonant reactions, the standard analytical approach is compared with the exact numerical treatment. Resonant reactions rates are illustrated by the 12C(p,?)13N reaction.
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