Sensitivity of Neutron-Rich Nuclear Isomer Behavior to Uncertainties in Direct Transitions

Misch, G. Wendell; Sprouse, Trevor; Mumpower, Matthew; Couture, A.; Fryer, Chris L.; Meyer, B. S.; Sun, Yang

doi:10.3390/sym13101831

Cited by 19 publications

(13 citation statements)

References 76 publications

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“…Additionally, nuclear physics models like FRDM2012 have a closed N = 126 shell far from stability, which in this simulation results in an overproduction of this peak relative to the solar residuals. Relevant nuclear physics uncertainties for r-process nucleosynthesis have been studied extensively in the works of Mumpower et al (2016b), Vassh et al (2019, Misch et al (2021), andMumpower et al (2022).…”

Section: Resultsmentioning

confidence: 99%

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: Resultsmentioning

confidence: 99%

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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“…However, 26 Al has several isomers that complicate the decay chain. The ground state of 26 Al decays to 26 Mg with a half-life of ∼700 kyr; however, the excited state of 26 Al decays to 26 Mg in ∼6 s (Misch et al 2021). At the temperatures found in stellar envelopes, excited 26 Al decays to 26 Mg before it can de-excite back to its ground state; this rapidly converts most of the 26 Al into 26 Mg. Our nuclear network does not contain the 26 Al isomers, with the decay rate of 26 Al only considering the ground-state transitions.…”

Section: Al26mentioning

confidence: 99%

Nucleosynthesis of Binary-stripped Stars

Farmer

Laplace

et al. 2023

ApJ

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The cosmic origin of the elements, the fundamental chemical building blocks of the universe, is still uncertain. Binary interactions play a key role in the evolution of many massive stars, yet their impact on chemical yields is poorly understood. Using the MESA stellar evolution code, we predict the chemical yields ejected in wind mass loss and the supernovae of single and binary-stripped stars. We do this with a large 162-isotope nuclear network at solar metallicity. We find that binary-stripped stars are more effective producers of the elements than single stars, due to their increased mass loss and an increased chance to eject their envelopes during a supernova. This increased production by binaries varies across the periodic table, with F and K being more significantly produced by binary-stripped stars than single stars. We find that the 12C/13C could be used as an indicator of the conservativeness of mass transfer, as 13C is preferentially ejected during mass transfer while 12C is preferentially ejected during wind mass loss. We identify a number of gamma-ray-emitting radioactive isotopes that may be used to help constrain progenitor and explosion models of core-collapse supernovae with next-generation gamma-ray detectors. For single stars we find that 44V and 52Mn are strong probes of the explosion model, while for binary-stripped stars it is 48Cr. Our findings highlight that binary-stripped stars are not equivalent to two single stars and that detailed stellar modeling is needed to predict their final nucleosynthetic yields.

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“…However, 26 Al has several isomers which complicate the decay chain. The ground state of 26 Al decays to 26 Mg with a half life of ∼ 700 kyr, however the excited state of 26 Al decays to 26 Mg in ∼ 6 seconds (Misch et al 2021). At the temperatures found in stellar envelopes, excited 26 Al decays to 26 Mg before it can de-excite back to its ground state, this rapidly converts most of the 26 Al into 26 Mg. Our nuclear network does not contain the 26 Al isomers, with the decay rate of 26 Al only considering the ground state transitions.…”

Section: Gamma Ray Emittersmentioning

confidence: 99%

Nucleosynthesis of binary-stripped stars

Farmer¹,

Laplace²,

Ma³

et al. 2023

Preprint

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The cosmic origin of the elements, the fundamental chemical building blocks of the Universe, is still uncertain. Binary interactions play a key role in the evolution of many massive stars, yet their impact on chemical yields is poorly understood. Using the MESA stellar evolution code we predict the chemical yields ejected in wind mass loss and the supernovae of single and binary-stripped stars. We do this with a large 162 isotope nuclear network at solar-metallicity. We find that binary-stripped stars are more effective producers of the elements than single stars, due to their increased mass loss and an increased chance to eject their envelopes during a supernova. This increased production by binaries varies across the periodic table, with F and K being more significantly produced by binary-stripped stars than single stars. We find that the 12 C/ 13 C could be used as an indicator of the conservativeness of mass transfer, as 13 C is preferentially ejected during mass transfer while 12 C is preferentially ejected during wind mass loss. We identify a number of gamma-ray emitting radioactive isotopes that may be used to help constrain progenitor and explosion models of core-collapse supernovae with next-generation gammaray detectors. For single stars we find 44 V and 52 Mn are strong probes of the explosion model, while for binary-stripped stars it is 48 Cr. Our findings highlight that binary-stripped stars are not equivalent to two single stars and that detailed stellar modelling is needed to predict their final nucleosynthetic yields.

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Sensitivity of Neutron-Rich Nuclear Isomer Behavior to Uncertainties in Direct Transitions

Cited by 19 publications

References 76 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

Nucleosynthesis of Binary-stripped Stars

Nucleosynthesis of binary-stripped stars

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