Direct Measurement of Resonances in 
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Psaltis, A.; Chen, A. A.; Longland, R.; Connolly, D.; Brune, C. R.; Davids, B.; Fallis, J.; Giri, R.; Greife, U.; Hutcheon, D.A.; Kroll, L.; Lennarz, A.; Liang, J. F.; Lovely, M.; Luo, M.; Marshall, C.; Paneru, S. N.; Parikh, A.; Ruiz, C.; Shotter, A.C.; Williams, M.

doi:10.1103/physrevlett.129.162701

Cited by 6 publications

(1 citation statement)

References 36 publications

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“…The astrophysical and nuclear physics uncertainties of the νp-process have been explored extensively by Wanajo et al (2011), Arcones et al (2012), andNishimura et al (2019), and these uncertainties have motivated new measurements of nuclear masses and thermonuclear reaction rates (e.g., Fallis et al 2011;Xing et al 2018;Randhawa et al 2021;Psaltis et al 2022b).…”

Section: νP-processmentioning

confidence: 99%

Neutrino-driven Outflows and the Elemental Abundance Patterns of Very Metal-poor Stars

Psaltis,

Jacobi,

Montes

et al. 2024

ApJ

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The elemental abundances between strontium and silver (Z = 38–47) observed in the atmospheres of very metal-poor stars in the Galaxy may contain the fingerprint of the weak r-process and ν p-process occurring in early core-collapse supernovae explosions. In this work, we combine various astrophysical conditions based on a steady-state model to cover the richness of the supernova ejecta in terms of entropy, expansion timescale, and electron fraction. The calculated abundances based on different combinations of conditions are compared with stellar observations, with the aim of constraining supernova ejecta conditions. We find that some conditions of the neutrino-driven outflows consistently reproduce the observed abundances of our sample. In addition, from the successful combinations, the neutron-rich trajectories better reproduce the observed abundances of Sr–Zr (Z = 38–40), while the proton-rich ones, Mo–Pd (Z = 42–47).

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