Synthesis of the Elements in Stars

Burbidge, E. M.; Burbidge, G. R.; Fowler, William A.; Hoyle, F.

doi:10.1103/revmodphys.29.547

Cited by 3,777 publications

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References 162 publications

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“…The half-life is an important factor in investigations into astrophysical environments and nuclear structure. For example, the formation of the third peak in observed solar r-process abundance patterns is dependent on the half-life [9,10]. Also, the abundance peak height around A = 195 is proportional to the half-life, and the peak position and its width drastically change according to the half-life.…”

Section: Introductionmentioning

confidence: 99%

In-gas-cell laser spectroscopy of the magnetic dipole moment of the N≈126 isotope Pt199

et al. 2017

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The magnetic dipole moment and mean-square charge radius of 199g Pt (I π = 5/2 − , t 1/2 = 30.8 min) ground state and 199m Pt (E ex = 424 keV, I π = (13/2) + , t 1/2 = 13.6 s) isomeric state are evaluated for the first time from investigations of the hyperfine splitting of the λ 1 = 248.792 nm transition by in-gas-cell laser ionization spectroscopy. Ground and isomeric states of neutron-rich 199 Pt nucleus were produced by a multinucleon transfer reaction at the KEK Isotope Separation System (KISS), designed for the study of nuclear spectroscopy in the vicinity of N = 126. The measured magnetic dipole moments +0.75(8)μ N and −0.57(5)μ N are consistent with the systematics of those of nuclei with I π = 5/2 − and I π = 13/2 + , respectively.

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Section: Introductionmentioning

confidence: 99%

In-gas-cell laser spectroscopy of the magnetic dipole moment of the N≈126 isotope Pt199

et al. 2017

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“…It has long been understood that nuclear masses are of key importance for r-process nucleosynthesis [1]. For an r process that proceeds in equilibrium between neutron captures and photodissociations, masses determine the relative abundances along each isotopic chain.…”

Section: Introductionmentioning

confidence: 99%

Systematic and Statistical Uncertainties in Simulated r-Process Abundances due to Uncertain Nuclear Masses

Surman¹,

Mumpower²,

McLaughlin³

2017

Proceedings of the 14th International Symposium on Nuclei in the Cosmos (NIC2016)

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Unknown nuclear masses are a major source of nuclear physics uncertainty for r-process nucleosynthesis calculations. Here we examine the systematic and statistical uncertainties that arise in r-process abundance predictions due to uncertainties in the masses of nuclear species on the neutron-rich side of stability. There is a long history of examining systematic uncertainties by the application of a variety of different mass models to r-process calculations. Here we expand upon such efforts by examining six DFT mass models, where we capture the full impact of each mass model by updating the other nuclear properties-including neutron capture rates, β-decay lifetimes, and β-delayed neutron emission probabilities-that depend on the masses. Unlike systematic effects, statistical uncertainties in the r-process pattern have just begun to be explored. Here we apply a global Monte Carlo approach, starting from the latest FRDM masses and considering random mass variations within the FRDM rms error. We find in each approach that uncertain nuclear masses produce dramatic uncertainties in calculated r-process yields, which can be reduced in upcoming experimental campaigns.

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“…Core-collapse SNe [5] and neutron star binary mergers are considered as possible sites [6][7][8]. The first produces small amounts of material at a high event rate while the latter produces large amounts in rare events.…”

Section: Introductionmentioning

confidence: 99%

Short-Lived ²⁴⁴Pu Points to Neutron Star Binary Mergers as Sites for r-Process Nucleosynthesis

Hotokezaka¹,

Piran²,

Paul³

2017

Proceedings of the 14th International Symposium on Nuclei in the Cosmos (NIC2016)

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Measurements of the radioactive 244 Pu abundances can break the degeneracy between high-rate/lowyield and low-rate/high-yield scenarios for the production of heavy r-process elements. The first corresponds to production by core collapse supernovae (cc-SNe) while the latter corresponds to production by e.g. neutron star binary mergers. The estimated 244 Pu abundance in the current interstellar medium inferred from deep-sea measurements is significantly lower than that corresponding Early Solar System abundances. We estimate the expected median value of the 244 Pu abundances and fluctuations around this value in both models [1]. We show that while the current and Early Solar System abundances are explained within the low-rate/high-yield scenario, they are incompatible with the high-rate/low-yield (cc-SNe) model. The inferred event rate remarkably agrees with neutron star binary merger rates estimated from Galactic neutron star binaries and from short gamma-ray bursts. The ejected mass of r-process elements per event agrees with both theoretical and observational macronova estimates.

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Synthesis of the Elements in Stars

Abstract: Synt iesis oI. ' t.~e. '~.

Cited by 3,777 publications

References 162 publications

In-gas-cell laser spectroscopy of the magnetic dipole moment of the N≈126 isotope Pt199

In-gas-cell laser spectroscopy of the magnetic dipole moment of the N≈126 isotope Pt199

Systematic and Statistical Uncertainties in Simulated r-Process Abundances due to Uncertain Nuclear Masses

Short-Lived ²⁴⁴Pu Points to Neutron Star Binary Mergers as Sites for r-Process Nucleosynthesis

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Synthesis of the Elements in Stars

Abstract: Synt iesis oI. ' t.~e. '~.

Cited by 3,777 publications

References 162 publications

In-gas-cell laser spectroscopy of the magnetic dipole moment of the N≈126 isotope Pt199

In-gas-cell laser spectroscopy of the magnetic dipole moment of the N≈126 isotope Pt199

Systematic and Statistical Uncertainties in Simulated r-Process Abundances due to Uncertain Nuclear Masses

Short-Lived 244Pu Points to Neutron Star Binary Mergers as Sites for r-Process Nucleosynthesis

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Short-Lived ²⁴⁴Pu Points to Neutron Star Binary Mergers as Sites for r-Process Nucleosynthesis