Constraining the destruction rate of 40K in stellar nucleosynthesis through the study of the 40Ar(p, n)40K reaction

Background:K- 40 plays a significant role in the radiogenic heating of Earth-like exoplanets, which can affect the development of a habitable environment on their surfaces. The initial amount of K-40 in the interior of these planets depends on the composition of the interstellar clouds from which they formed. Within this context, nuclear reactions that regulate the production of K-40 during stellar evolution can play a critical role. Purpose: In this study, we constrain for the first time the astrophysical reaction rate of K-40(n, p)Ar-40 which is responsible for the destruction of K-40 during stellar nucleosynthesis. We provide to the nuclear physics community high-resolution data on the cross section and angular distribution of the Ar-40(p, n)K-40 reaction. These are important to various applications involving Ar-40. The associated reaction rate of the( 40)Ar(p, n)K-40 process addresses a reaction rate gap in the Joint Institute for Nuclear Astrophysics REACLIB database in the region of intermediate-mass isotopes. Methods: We performed differential cross-section measurements on the Ar-40(p, n)K-40 reaction, for six energies in the center-of-mass system between 3.2 and 4.0 MeV and various angles between 0 degrees and 135 degrees. The experiment took place at the Edwards Accelerator Laboratory at Ohio University using the beam swinger target location and a standard neutron time-of-flight technique. We extracted total and partial cross sections by integrating the double differential cross sections we measured. Results: The total and partial cross sections varied with energy due to the contribution from isobaric analog states and Ericson type fluctuations. The energy-averaged neutron angular distributions were symmetrical relative to 90 degrees. Based on the experimental data, local transmission coefficients were extracted and were used to calculate the astrophysical reaction rates of Ar-40(p, n)K-40 and K-40(n, p)Ar-40 reactions. The new rates were found to vary significantly from the theoretical rates in the REACLIB library. We implemented the new rates in network calculations to study nucleosynthesis via the slow neutron capture process, and we found that the produced abundance of K-40 is reduced by up to 10% compared to calculations with the library rates. At the same time, the above result removes a significant portion of the previous theoretical uncertainty on the K-40 yields from stellar evolution calculations. Conclusions: Our results support a destruction rate of K-40 in massive stars via the K-40(n, p)Ar-40 reaction that is larger compared to previous estimates. The rate of 40 K destruction via the K-40(n, p)Ar-40 reaction now has a dramatically reduced uncertainty based on our measurement. This result directly affects the predicted stellar yields of K-40 from nucleosynthesis, which is a critical input parameter for the galactic chemical evolution models that are currently employed for the study of significant properties of exoplanets.