Abstract
Nuclear masses play a central role in nuclear astrophysics, significantly impacting the origin of the elements and observables used to constrain ultradense matter. A variety of techniques are available to meet this need, varying in their emphasis on precision and reach from stability. Here I briefly summarize the status of and near-future for the time-of-flight magnetic-rigidity (TOF-Bρ) mass measurement technique, emphasizing the complementary and interconnectedness with higher-precision mass measurement methods. This includes of recent examples from TOF-Bρ mass measurements that map the evolution of nuclear structure across the nuclear landscape and significantly impact the results and interpretation of astrophysical model calculations. I also forecast expected expansion in the known nuclear mass surface from future measurement at the Facility for Rare Isotope Beams.
Highlights
IntroductionNuclear mass differences, are fundamental descriptors of atomic nuclei
Nuclear masses, and nuclear mass differences, are fundamental descriptors of atomic nuclei
Mass differences reflect the evolving energetics associated with changes in nuclear structure across the nuclear landscape as well as the energy costs for nuclear reactions in astrophysical environments
Summary
Nuclear mass differences, are fundamental descriptors of atomic nuclei. Recent contributions include the emergence of the N = 32 [1] and N = 34 shell closures [2], mapping the island of inversion near N = 40 [3], Q-value determinations essential for calculations of type-I X-ray bursts [4, 5], and determining the trend in masses of neutron rich nuclei whose imprint can be seen in calculations of astrophysical r-process abundance patterns [6, 7] In all of these cases, precise nuclear mass determinations were required to contribute to solving the problem at hand.
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