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The production of s-isotopes due to the operation of the reaction ¹³C(α, n)¹⁶O in low-mass stars during asymptotic giant branch phases is investigated following in detail the time evolution of the thermal pulses, the temperature and density stratification within the convective shells, and taking into account the effect of the neutron recycling by ¹²C through the chain ¹²C(n, γ)¹³C(α, n)¹⁶O. The resulting average neutron density reaches a maximum of about 5×10⁹cm⁻³ and then decreases smoothly. Strong overabundances for all s-isotopes with A > 80 are obtained in a solar system distribution. The process appears suitable to reproduce many observed details concerning isotopic ratios.
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Gallino et al. (1988) studied this question.
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