Within the context of the proton–neutron quasi-particle random phase approximation (pn-QRPA) model and TALYS v1.96 code, the radiative capture (99Tc(n, γ)100Tc) and stellar weak interaction (99Tc → 99Ru + e− + νe) rates were computed during thermal pulses operating in asymptotic giant branch stars. The Maxwellian average cross-section (MACS) and neutron capture rates for the 99Tc(n, γ)100Tc process are analyzed within the context of statistical code TALYS v1.96. The effect of nuclear level density (NLD) and γ-strength functions on MACS and neutron capture rates has been examined. The model-based computations for MACS provided an insightful contrast to prior investigated findings. The sensitivity of stellar weak interaction rates to different densities and temperatures is investigated using the pn-QRPA model. The impact of thermally populated excited states on electron emission (β−) rates in 99Tc is extensively examined. Additionally, a comparison is made between the study of the stellar β−decay rates and the thermal neutron capture rates. It is found that at T9 = 0.26 the thermal neutron capture rates (λ(n, γ)) and the temperature dependent stellar β−decay rates () cross each other. However, at higher temperatures, the λ(n, γ) are found to be higher than .

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