Examination of Radiative Capture Rates of ⁹⁹Tc(<i>n</i>, <i>γ</i>) ¹⁰⁰Tc and Stellar <i>β</i> ⁻ Decay Rates of ⁹⁹Tc

Abstract Within the context of the proton–neutron quasi-particle random phase approximation (pn-QRPA) model and TALYS v1.96 code, the radiative capture ( 99 Tc( n , γ ) 100 Tc) and stellar weak interaction ( 99 Tc → 99 Ru + e − + ν e ) rates were computed during thermal pulses operating in asymptotic giant branch stars. The Maxwellian average cross-section (MACS) and neutron capture rates for the 99 Tc( n , γ ) 100 Tc 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 99 Tc 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 T 9 = 0.26 the thermal neutron capture rates ( λ ( n , γ ) ) and the temperature dependent stellar β − decay rates ( <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> <mml:msub> <mml:mrow> <mml:mi>λ</mml:mi> </mml:mrow> <mml:mrow> <mml:msup> <mml:mrow> <mml:mi>β</mml:mi> </mml:mrow> <mml:mrow> <mml:mo>−</mml:mo> </mml:mrow> </mml:msup> </mml:mrow> </mml:msub> </mml:math> ) cross each other. However, at higher temperatures, the λ ( n , γ ) are found to be higher than <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> <mml:msub> <mml:mrow> <mml:mi>λ</mml:mi> </mml:mrow> <mml:mrow> <mml:msup> <mml:mrow> <mml:mi>β</mml:mi> </mml:mrow> <mml:mrow> <mml:mo>−</mml:mo> </mml:mrow> </mml:msup> </mml:mrow> </mml:msub> </mml:math> .