First Application of Mass Measurements with the Rare-RI Ring Reveals the Solar 
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-Process Abundance Trend at 
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Li, H F; Naimi, S.; Sprouse, Trevor; Mumpower, Matthew; Abe, Yasushi; Yamaguchi, Yoshitaka; Nagae, D.; Suzaki, F.; Wakasugi, M.; Arakawa, Hiroshi; Wang, D.; D., Hamakawa,; Hosoi, S.; Inada, Y.; Kajiki, D; Kobayashi, Takaaki; Sakaue, Mamoru; Yokoda, Y; Yamaguchi, Takayuki; Kagesawa, R.; Kamioka, Daiki; Moriguchi, T.; Mukai, M.; Ozawa, A.; Ota, S.; Kitamura, N.; Masuoka, S.; Michimasa, S.; Baba, H.; Fukuda, N.; Shimizu, Y.; Suzuki, Hiroshi; Takeda, Hiroyuki; Ahn, D. S.; Wang, M; Fu, Chuancheng; Wang, Q; Suzuki, Shinji; Zhuang, G.; Litvinov, Yu. A.; Lorusso, G.; Walker, P. M.; Podolyák, Zs.; Uesaka, T.

doi:10.1103/physrevlett.128.152701

Cited by 20 publications

(4 citation statements)

References 44 publications

(58 reference statements)

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“…This situation arises naturally from the simulation and thus means the conditions under which heavy element synthesis proceeds will also show large variation. Our results thus highlight the need for future nuclear sensitivity studies to cover a wide range of conditions, as shown in the recent work of Li et al (2022).…”

Section: From Tracer To Trajectorysupporting

confidence: 72%

Emergent Nucleosynthesis from a 1.2 s Long Simulation of a Black Hole Accretion Disk

Sprouse,

Lund,

Miller

et al. 2024

ApJ

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We simulate a black hole accretion disk system with full-transport general relativistic neutrino radiation magnetohydrodynamics for 1.2 s. This system is likely to form after the merger of two compact objects and is thought to be a robust site of r-process nucleosynthesis. We consider the case of a black hole accretion disk arising from the merger of two neutron stars. Our simulation time coincides with the nucleosynthesis timescale of the r-process (∼1 s). Because these simulations are time-consuming, it is common practice to run for a “short” duration of approximately 0.1–0.3 s. We analyze the nucleosynthetic outflow from this system and compare the results of stopping at 0.12 and 1.2 s. We find that the addition of mass ejected in the longer simulation as well as more favorable thermodynamic conditions from emergent viscous ejecta greatly impacts the nucleosynthetic outcome. We quantify the error in nucleosynthetic outcomes between short and long cuts.

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Section: From Tracer To Trajectorysupporting

confidence: 72%

Emergent Nucleosynthesis from a 1.2 s Long Simulation of a Black Hole Accretion Disk

Sprouse,

Lund,

Miller

et al. 2024

ApJ

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“…These discrepancies could signal the need for further improvements in nuclear structure models, and nuclear masses in particular, for nuclei just below the A ∼ 130 peak (see Kratz et al 2014). For example, the Sn and Sb behavior is consistent with a recent measurement by Li et al (2022) that improved the uncertainty on the mass of the neutron-rich isotope 123 Pd. That measurement implies a slight decrease in the r-process abundance of the A = 123 isobar, which is linked to one of only two stable Sb isotopes.…”

Section: The Second R-process Peakmentioning

confidence: 55%

The R-process Alliance: A Nearly Complete R-process Abundance Template Derived from Ultraviolet Spectroscopy of the R-process-enhanced Metal-poor Star HD 222925*

Roederer

Lawler

Hartog

et al. 2022

ApJS

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We present a nearly complete rapid neutron-capture process (r-process) chemical inventory of the metal-poor ([Fe/H] = −1.46 ± 0.10) r-process-enhanced ([Eu/Fe] = +1.32 ± 0.08) halo star HD 222925. This abundance set is the most complete for any object beyond the solar system, with a total of 63 metals detected and seven with upper limits. It comprises 42 elements from 31 ≤ Z ≤ 90, including elements rarely detected in r-process-enhanced stars, such as Ga, Ge, As, Se, Cd, In, Sn, Sb, Te, W, Re, Os, Ir, Pt, and Au. We derive these abundances from an analysis of 404 absorption lines in ultraviolet spectra collected using the Space Telescope Imaging Spectrograph on the Hubble Space Telescope and previously analyzed optical spectra. A series of appendices discusses the atomic data and quality of fits for these lines. The r-process elements from Ba to Pb, including all elements at the third r-process peak, exhibit remarkable agreement with the solar r-process residuals, with a standard deviation of the differences of only 0.08 dex (17%). In contrast, deviations among the lighter elements from Ga to Te span nearly 1.4 dex, and they show distinct trends from Ga to Se, Nb through Cd, and In through Te. The r-process contribution to Ga, Ge, and As is small, and Se is the lightest element whose production is dominated by the r-process. The lanthanide fraction, log X La = −1.39 ± 0.09, is typical for r-process-enhanced stars and higher than that of the kilonova from the GW170817 neutron-star merger event. We advocate adopting this pattern as an alternative to the solar r-process-element residuals when confronting future theoretical models of heavy-element nucleosynthesis with observations.

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“…The mass of the nucleus is one of the most crucial ingredients on which many nuclear properties depend. Although great experimental progress has been made in the last decades to reach the exotic neutronrich region and future large facilities such as the Facility for Rare Isotope Beams (FRIBs; Surman & Mumpower 2018 ), the Facility for Antiproton and Ion Research (FAIR; Walker, Litvinov & Geissel 2013 ), and the Radioactive Isotope Beam Factory (RIBF) at RIKEN (Li et al 2022 ) will certainly help to pro vide e xperimental masses deep inside the neutron-rich region, it will not be feasible to measure the masses of the nuclei of most importance to the r-process in the years to come. Thus, our nucleosynthesis calculations will have to continue to rely on theoretical masses in the foreseeable future.…”

Section: Nuclear Mass Modelsmentioning

confidence: 99%

Impact of systematic nuclear uncertainties on composition and decay heat of dynamical and disc ejecta in compact binary mergers

Kullmann

Goriely

Just

et al. 2023

Monthly Notices of the Royal Astronomical Society

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Theoretically predicted yields of elements created by the rapid neutron capture (r-) process carry potentially large uncertainties associated with incomplete knowledge of nuclear properties and approximative hydrodynamical modelling of the matter ejection processes. We present an in-depth study of the nuclear uncertainties by varying theoretical nuclear input models that describe the experimentally unknown neutron-rich nuclei. This includes two frameworks for calculating the radiative neutron capture rates and 14 different models for nuclear masses, β-decay rates and fission properties. Our r-process nuclear network calculations are based on detailed hydrodynamical simulations of dynamically ejected material from NS-NS or NS-BH binary mergers plus the secular ejecta from BH-torus systems. The impact of nuclear uncertainties on the r-process abundance distribution and the early radioactive heating rate is found to be modest (within a factor of ∼20 for individual A > 90 abundances and a factor of 2 for the heating rate). However, the impact on the late-time heating rate is more significant and depends strongly on the contribution from fission. We witness significantly higher sensitivity to the nuclear physics input if only a single trajectory is used compared to considering ensembles with a much larger number of trajectories (ranging between 150 and 300), and the quantitative effects of the nuclear uncertainties strongly depend on the adopted conditions for the individual trajectory. We use the predicted Th/U ratio to estimate the cosmochronometric age of six metal-poor stars and find the impact of the nuclear uncertainties to be up to 2 Gyr.

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First Application of Mass Measurements with the Rare-RI Ring Reveals the Solar r -Process Abundance Trend at A=122 and A=123

Cited by 20 publications

References 44 publications

Emergent Nucleosynthesis from a 1.2 s Long Simulation of a Black Hole Accretion Disk

Emergent Nucleosynthesis from a 1.2 s Long Simulation of a Black Hole Accretion Disk

The R-process Alliance: A Nearly Complete R-process Abundance Template Derived from Ultraviolet Spectroscopy of the R-process-enhanced Metal-poor Star HD 222925*

Impact of systematic nuclear uncertainties on composition and decay heat of dynamical and disc ejecta in compact binary mergers

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