Modification of nuclear transitions in stellar plasma by electronic processes:<mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" display="inline"><mml:mrow><mml:mi>K</mml:mi></mml:mrow></mml:math>isomers in<mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" display="inline"><mml:mmultiscripts><mml:mi mathvariant="normal">Lu</mml:mi><mml:mprescripts /><mml:none /><mml:mrow><mml:mn>176</mml:mn></mml:mrow></mml:mmultiscripts></mml:math>and<mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" dis

Gosselin, G.; Morel, Pascal; Mohr, P.

doi:10.1103/physrevc.81.055808

Cited by 13 publications

(16 citation statements)

References 54 publications

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“…This is the energy region where the plasma effects become important. The full formalism for the calculation of stellar reaction rates is given in an earlier work (Gosselin et al, 2010). The essential result is that the stellar reaction rate λ * for transitions from the low-K to the high-K states (and reverse) can be derived by a formula similar to Eq.…”

Section: Stellar Transition Ratesmentioning

confidence: 99%

“…As a rule of thumb, every transition with an energy lower than 100 keV must be looked at, as internal 6 conversion can significantly contribute to the transition rate. Some examples for several -transition energies have already been shown earlier (Gosselin et al, 2010). The two levels involved need not include the ground state, but can also be built on an isomeric state.…”

Section: Modification Of a Particular Transitionmentioning

confidence: 99%

“…The dominating effect is NEEC in this case. However, the modification of the stellar transition rate remains far below a factor of two in the astrophysically relevant energy region (Gosselin et al, 2010).…”

Section: Lu In the Astrophysical S-processmentioning

confidence: 99%

“…Enhancements of the radiative strength of up to a factor of 10 for this transition have been calculated (Gosselin et al, 2010) which are mainly based on NEEC. However, unfortunately the influence on the stellar transition rate between low-K states and high-K states remains very small.…”

Section: Ta and Its Uncertain Nucleosynthetic Originmentioning

confidence: 99%

“…At least four different electromagnetic excitation processes may be able to excite a nucleus under typical astrophysical plasma conditions (Gosselin et al, 2010):…”

Section: Modification Of a Particular Transitionmentioning

confidence: 99%

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Nuclear Excitation Processes in Astrophysical Plasmas

Gosselin¹,

Mohr²,

Méot³

et al. 2012

Astrophysics

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Section: Stellar Transition Ratesmentioning

confidence: 99%

Section: Modification Of a Particular Transitionmentioning

confidence: 99%

Section: Lu In the Astrophysical S-processmentioning

confidence: 99%

Section: Ta and Its Uncertain Nucleosynthetic Originmentioning

confidence: 99%

“…At least four different electromagnetic excitation processes may be able to excite a nucleus under typical astrophysical plasma conditions (Gosselin et al, 2010):…”

Section: Modification Of a Particular Transitionmentioning

confidence: 99%

See 3 more Smart Citations

Nuclear Excitation Processes in Astrophysical Plasmas

Gosselin¹,

Mohr²,

Méot³

et al. 2012

Astrophysics

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Astronuclear Physics: A tale of the atomic nuclei in the skies

Arnould

Goriely

2020

Progress in Particle and Nuclear Physics

108

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A century ago, nuclear physics entered astrophysics, giving birth to a new field of science referred to as "Nuclear Astrophysics". With time, it developed at an impressive pace into a vastly inter-and multidisciplinary discipline bringing into its wake not only astronomy and cosmology, but also many other sub-fields of physics, especially particle, solid-state and computational physics, as well as chemistry, geology and even biology. The present Astronuclear Physics review focusses primarily on the facets of nuclear physics that are of relevance to astronomy and astrophysics, the theoretical aspects being of special concern here. The observational aspects of astronomy and astrophysics that may have some connection to nuclear physics are only broadly reviewed, mainly through the provision of recent relevant references. Multi-messenger astronomy has developed most remarkably during the last decades, with often direct implications for nuclear astrophysics. The electromagnetic view of the components of the Universe has improved dramatically at all wavelengths, from the γ-ray to the radio domains, providing important new information on the Big Bang and the properties of stars. Neutrino astronomy has made giant steps forward. In particular, the famed "solar neutrino problem" is now behind us. The long-sought gravitational waves have at last been detected, with direct relevance namely to the merger of compact stars. The composition of Galactic Cosmic Rays and stellar/solar energetic particles is better known than ever, providing constrains on the GCR physics.On the stellar modeling side, we broadly brush the progress that has been made based on new observations, and even more so on the spectacular increase in computer capabilities. We briefly outline recent advances regarding the quiescent evolution of stars, as well as the eventual catastrophic supernova explosion of certain classes of them. In spite of significant improvements in the simulations, many long-standing problems still await solid solutions, particularly regarding the details and robustness of explosion simulations. In fact, new questions are continuously emerging, and new facts may endanger old ideas.The lion's share of this review concerns the nuclear physics phenomena that may be at work in astrophysical conditions, with a strong focus on theory. Exceptionally large varieties of nuclei have to be dealt with, ranging from the lightest to the heaviest ones, from the valley of nuclear stability all the way to the proton and neutron drip lines. An additional serious difficulty comes from the fact that the nuclei are immersed in highly unusual environments which may have a significant impact on their static properties, the diversity of their transmutation modes, some of which not being observable in the laboratory, and on the probabilities of these modes. The description of nuclei as individual entities has even to be replaced by the construction of an Equation of State at high enough temperatures and/or densities prevailing in the cores of exploding stars an...

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Simulation of nuclear isomer production in laser-induced plasma

Ma,

Wang,

Yang

et al. 2024

Matter and Radiation at Extremes

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Nuclear isomers play essential roles in various fields, including stellar nucleosynthesis, nuclear clocks, nuclear batteries, clean nuclear energy, and γ-ray lasers. Recent technological advances in high-intensity lasers have made it possible to excite or de-excite nuclear isomers using table-top laser equipment. Utilizing a particle-in-cell code, we investigate the interaction of a laser with a nanowire array and calculate the production rates of the 73mGe (E1 = 13.3 keV) and 107mAg (E1 = 93.1 keV) isomers. For 73m1Ge, production by Coulomb excitation is found to contribute a peak efficiency of 1.0 × 1019 particles s−1 J−1, while nuclear excitation by electron capture (NEEC) contributes a peak of 1.65 × 1011 particles s−1 J−1. These results indicate a high isomeric production ratio, as well as demonstrating the potential for confirming the existence of NEEC, a long-expected but so far experimentally unobserved fundamental process.

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Modification of nuclear transitions in stellar plasma by electronic processes:Kisomers inLu176and

Cited by 13 publications

References 54 publications

Nuclear Excitation Processes in Astrophysical Plasmas

Nuclear Excitation Processes in Astrophysical Plasmas

Astronuclear Physics: A tale of the atomic nuclei in the skies

Simulation of nuclear isomer production in laser-induced plasma

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