L. Balliet
Current Organizations / Institutes
The organizations/institutes from the scholar's latest article
Research Subjects
L. Balliet has a total of 63 co-authors. Here are the top co-authors by number of shared publications:
- Fernando Montes
National Superconducting Cyclotron Laboratory
2 shared publications - H. Arora
Panjab University
2 shared publications - R. Jain
Lawrence Livermore National Laboratory
2 shared publications - A. A. Doetsch
Facility for Rare Isotope Beams
1 shared publication - A. C. C. Villari
Facility for Rare Isotope Beams
1 shared publication A. Henriques
Facility for Rare Isotope Beams
1 shared publication
Latest Publications
- Open Access
Direct Measurement of the $^{59}$Cu$(p,α)^{56}$Ni Excitation Function to Constrain the Ni--Cu Cycle Strength and Its Impact on Explosive Nucleosynthesis
A new direct measurement of the $^{59}$Cu$(p,α){}^{56}$Ni excitation function from 2.43 to 5.88~MeV in the center-of-mass frame was performed in inverse kinematics using the high-efficiency MUSIC active-target detector at FRIB. This reaction plays a critical role in constraining the strength of the Ni--Cu cycle in explosive astrophysical environments such as Type~I X-ray bursts and the $ν$p-process in neutrino-driven winds following core-collapse supernovae. The newly derived stellar reaction rate is systematically lower than the REACLIB evaluation, resulting in less than 0.1\% recycling through the Ni--Cu cycle in X-ray bursts and an enhanced efficiency of the $ν$p-process up to temperatures of $T_9 \approx 3.7$.Open AccessDirect Measurement of the $^{59}$Cu$(p,α)^{56}$Ni Excitation Function to Constrain the Ni--Cu Cycle Strength and Its Impact on Explosive Nucleosynthesis
A new direct measurement of the $^{59}$Cu$(p,α){}^{56}$Ni excitation function from 2.43 to 5.88~MeV in the center-of-mass frame was performed in inverse kinematics using the high-efficiency MUSIC active-target detector at FRIB. This reaction plays a critical role in constraining the strength of the Ni--Cu cycle in explosive astrophysical environments such as Type~I X-ray bursts and the $ν$p-process in neutrino-driven winds following core-collapse supernovae. The newly derived stellar reaction rate is systematically lower than the REACLIB evaluation, resulting in less than 0.1\% recycling through the Ni--Cu cycle in X-ray bursts and an enhanced efficiency of the $ν$p-process up to temperatures of $T_9 \approx 3.7$. - 20 November 2025
- Published by American Physical Society (APS) in Physical Review Letters
- Vol. 135 (21) , 212701
Constraining the Synthesis of the Lightest p Nucleus Se 74
We provide the first experimental cross section of the ^{73}As(p,γ)^{74}Se reaction to constrain one of the main destruction mechanisms of the p nucleus ^{74}Se in explosive stellar environments. The measurement was done using a radioactive ^{73}As beam at effective center-of-mass energies of 2.9 and 2.3 MeV/nucleon. Along with the total cross-section measurement, statistical properties of the ^{74}Se compound nucleus were extracted, constraining the reaction cross section in the upper Gamow window of the γ process. The impact of the experimentally constrained reaction rate on ^{74}Se production in Type II supernovae was investigated through Monte Carlo one-zone network simulations. The results indicate that the overproduction of ^{74}Se by Type II supernova models cannot be resolved by nuclear physics alone and point toward the need for a more detailed understanding of the astrophysical conditions of relevance for the γ process.
- 20 November 2025
- Published by American Physical Society (APS) in Physical Review Letters
- Vol. 135 (21) , 212701
Constraining the Synthesis of the Lightest p Nucleus Se 74
We provide the first experimental cross section of the ^{73}As(p,γ)^{74}Se reaction to constrain one of the main destruction mechanisms of the p nucleus ^{74}Se in explosive stellar environments. The measurement was done using a radioactive ^{73}As beam at effective center-of-mass energies of 2.9 and 2.3 MeV/nucleon. Along with the total cross-section measurement, statistical properties of the ^{74}Se compound nucleus were extracted, constraining the reaction cross section in the upper Gamow window of the γ process. The impact of the experimentally constrained reaction rate on ^{74}Se production in Type II supernovae was investigated through Monte Carlo one-zone network simulations. The results indicate that the overproduction of ^{74}Se by Type II supernova models cannot be resolved by nuclear physics alone and point toward the need for a more detailed understanding of the astrophysical conditions of relevance for the γ process.