Abstract
Radiative capture reaction rates for $^6$He, $^9$Be and $^{17}$Ne formation at astrophysical conditions are studied within a three-body model using the analytical transformed harmonic oscillator method to calculate their states. An alternative procedure to estimate these rates from experimental data on low-energy breakup is also discussed
Highlights
Radiative capture reactions are crucial for the stellar models aiming to describe the evolution in composition, energy production and temperature structure of different astrophysical environments [1]
Three-body radiative capture processes are essential in overcoming the A = 5, 8 instability gaps, and traditionally they have been described as two-step sequential reactions [4]
Radiative capture reaction rates can be obtained from the inverse photodissociation cross section, which can be calculated within a proper three-body model for the compound nucleus [6]
Summary
Radiative capture reactions are crucial for the stellar models aiming to describe the evolution in composition, energy production and temperature structure of different astrophysical environments [1]. Reaction cross sections may not be measured directly This may occur if the initial nucleus is exotic [2], or when the capture process is a three-body reaction [3]. Three-body radiative capture processes are essential in overcoming the A = 5, 8 instability gaps, and traditionally they have been described as two-step sequential reactions [4]. Radiative capture reaction rates can be obtained from the inverse photodissociation cross section, which can be calculated within a proper three-body model for the compound nucleus [6]. We summarize some recent results on three-body capture reactions and discuss future developments
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