Nuclear astrophysics at FRANZ

Reifarth, R.; Dababneh, S.; Fiebiger, Stefan; Glorius, J.; Göbel, K.; Heil, M.; Hillmann, Paula; Heftrich, T.; Langer, C.; Meusel, O.; Plag, R.; Schmidt, S.; Slavkovská, Z.; Veltum, Daniel; Weigand, M.; Wiesner, Christoph; Wolf, C.; Zadeh, Ashkan Taremi

doi:10.1088/1742-6596/940/1/012024

Cited by 4 publications

(2 citation statements)

References 21 publications

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“…3, lower panel, shows that its uncertainty is only propagated locally to the isotopes affected by the branching point, i.e., 86 Kr, the Rb isotopes and the s-only isotopes 86 Sr and 87 Sr. Therefore, while the total impact of 85 Kr(n,γ ) 86 Kr is limited (it does not appear in the rate list in Table 2), robust s-process predictions in the Kr-Sr region need more precise data for this (challenging) reaction rate from the next generation of experimental facilities [71].…”

Section: Results Of the Nuclear Sensitivity Studymentioning

confidence: 99%

The s process in massive stars, a benchmark for neutron capture reaction rates

Pignatari,

Gallino,

Reifarth

2023

Eur. Phys. J. A

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A clear definition of the contribution from the slow neutron-capture process (s process) to the solar abundances between Fe and the Sr-Zr region is a crucial challenge for nuclear astrophysics. Robust s-process predictions are necessary to disentangle the contribution from other stellar processes producing elements in the same mass region. Nuclear uncertainties are affecting s-process calculations, but most of the needed nuclear input are accessible to present nuclear experiments or they will be in the near future. Neutron-capture rates have a great impact on the s process in massive stars, which is a fundamental source for the solar abundances of the lighter s-process elements heavier than Fe (weak s-process component). In this work we present a new nuclear sensitivity study to explore the impact on the s process in massive stars of 86 neutron-capture rates, including all the reactions between C and Si and between Fe and Zr. We derive the impact of the rates at the end of the He-burning core and at the end of the C-burning shell, where the $$^{22}$$ 22 Ne($$\alpha $$ α ,n)$$^{25}$$ 25 Mg reaction is is the main neutron source. We confirm the relevance of the light isotopes capturing neutrons in competition with the Fe seeds as a crucial feature of the s process in massive stars. For heavy isotopes we study the propagation of the neutron-capture uncertainties, finding a clear difference of the impact of Fe and Co isotope rates with respect to the rates of heavier stable isotopes. The local uncertainty propagation due to the neutron-capture rates at the s-process branching points is also considered, discussing the example of $$^{85}$$ 85 Kr. The complete results of our study for all the 86 neutron-capture rates are available online. Finally, we present the impact on the weak s process of the neutron-capture rates included in the new ASTRAL library (v0.2).

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Section: Results Of the Nuclear Sensitivity Studymentioning

confidence: 99%

The s process in massive stars, a benchmark for neutron capture reaction rates

Pignatari,

Gallino,

Reifarth

2023

Eur. Phys. J. A

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“…In carrying out innovations in the fields of education and research, every educator and researcher needs to instill an awareness of the importance of cooperation in advancing the field of astronomy. One of the innovative efforts that can be made is to apply the concept of astronomy with the help of technology that is cheap, easy to obtain, accessible, and operated by students [4,5]. This ensures that the quality of education in developing countries remains competitive with that in developed nations.…”

Section: Introductionmentioning

confidence: 99%

Visualization of Mercury's Orbital Path Around the Sun Using Matlab for Astronomic Distance Learning

2024

JJP

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Physical phenomena occurring at both macro and micro scales are often beyond direct observation by the human senses. This study aims to present an alternative astronomical learning activity about the orbital trajectory of the planet Mercury around the Sun using MATLAB assistance. Visualization of the orbital trajectory of Mercury begins by describing the appropriate mathematical equations. Subsequently, these equations are translated into graphical representations using MATLAB for visualization. In this study, students can visualize the orbital trajectory of Mercury around the Sun using MATLAB by varying the components of the coordinate equation. Through this visualization, it is hoped that it can help students understand the movement of Mercury around the Sun in its orbit independently and creatively. Students can also develop mathematical representation skills and visual representations of the orbital trajectory of Mercury around the Sun. Keywords: Astronomic, Distance Learning, MATLAB, Mercury, Orbit.

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Neutron capture cross section of $$^{83}$$Kr

Fiebiger

Baramsai²,

Couture³

et al. 2023

Eur. Phys. J. A

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The neutron capture cross section of $$^{83}$$ 83 Kr has been measured via the time-of-flight technique between 25 meV and 500 keV. The experiment used the DANCE array at the Los Alamos National Laboratory. Maxwellian Averaged Cross Sections have been derived for a range of stellar temperatures and are found to be in good agreement with previous data. The impact of the new cross sections on stellar nucleosynthesis has been investigated.

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Nuclear astrophysics at FRANZ

Cited by 4 publications

References 21 publications

The s process in massive stars, a benchmark for neutron capture reaction rates

The s process in massive stars, a benchmark for neutron capture reaction rates

Visualization of Mercury's Orbital Path Around the Sun Using Matlab for Astronomic Distance Learning

Neutron capture cross section of $$^{83}$$Kr

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