Nucleosynthesis of Light Elements and Heavy<i>r</i>‐Process Elements through the ν‐Process in Supernova Explosions

Yoshida, Takashi; Terasawa, M.; Kajino, Toshitaka; Sumiyoshi, Kohsuke

doi:10.1086/379766

Cited by 67 publications

(124 citation statements)

References 59 publications

Supporting

Mentioning

121

Contrasting

Order By: Relevance

“…The "light" ν-process involves interactions among neutrinos and lighter nuclei in core-collapse supernovae (CCSNe) environments (Woosley et al 1990;Yoshida et al 2004;Heger et al 2005). The neutrinos elevate nuclei to excited states, which then decay by nucleon emission (Hartmann et al 1991).…”

Section: ν-Processmentioning

confidence: 99%

Metallicity-Dependent Galactic Isotopic Decomposition for Nucleosynthesis

West

Heger

2013

ApJ

View full text Add to dashboard Cite

All stellar evolution models for nucleosynthesis require an initial isotopic abundance set to use as a starting point. Generally, our knowledge of isotopic abundances of stars is fairly incomplete except for the Sun. We present a first model for a complete average isotopic decomposition as a function of metallicity. Our model is based on the underlying nuclear astrophysics processes, and is fitted to observational data, rather than traditional forward galactic chemical evolution modeling which integrates stellar yields beginning from big bang nucleosynthesis. We first decompose the isotopic solar abundance pattern into contributions from astrophysical sources. Each contribution is then assumed to scale as a function of metallicity. The resulting total isotopic abundances are summed into elemental abundances and fitted to available halo and disk stellar data to constrain the model's free parameter values. This procedure allows us to use available elemental observational data to reconstruct and constrain both the much needed complete isotopic evolution that is not accessible to current observations, and the underlying astrophysical processes. As an example, our model finds a best fit for Type Ia contributing 0.7 to the solar Fe abundance, and Type Ia onset occurring at [Fe/H] −1.1, in agreement with typical values.

show abstract

Section: ν-Processmentioning

confidence: 99%

Metallicity-Dependent Galactic Isotopic Decomposition for Nucleosynthesis

West

Heger

2013

ApJ

View full text Add to dashboard Cite

show abstract

“…We adopt the same stellar model as that described in [3,4,6,7]. The SN progenitor is a 16.2 M star [8], and the explosion is followed numerically with a piecewise parabolic method [9].…”

Section: Supernova Nucleosynthesis Model and Neutrino Parametersmentioning

confidence: 99%

“…We set the explosion energy and the mass cut to be 1 × 10 51 ergs and 1.61 M , respectively. Detailed explosive nucleosynthesis is calculated by postprocessing using a nuclear reaction network including 291 species of nuclei [3].…”

Section: Supernova Nucleosynthesis Model and Neutrino Parametersmentioning

confidence: 99%

“…We will discuss the effect of uncertainties in the total neutrino energy and the neutrino temperatures [6,7]. The ν-process cross sections are adopted from [10] except charged-current reactions of 4 He and 12 C: 4 He(ν e , e − p) 3 He, 4 He(ν e , e + n) 3 H, 12 C(ν e , e − p) 11 C, and 12 C(ν e , e + n) 11 B. In this study, we focus on the change of the rates of these reactions due to neutrino oscillations because the ν-process reactions of 4 He and 12 C are the most important for 7 Li and 11 B production.…”

Section: Supernova Nucleosynthesis Model and Neutrino Parametersmentioning

confidence: 99%

“…The resulting large neutrino irradiation of the stellar layers above the PNS induces significant modifications of the isotopic abundance patterns, which is referred to as the ν-process. This process plays an important role for the production of, amongst several, the light elements 7 Li and 11 B [2,3,4]. On the other hand, it has been shown that the neutrinos change their flavors in the O/C and He-rich layers and that this flavor change strongly depends on the mass hierarchy and the mixing angle θ 13 (e.g., [5]).…”

Section: Introductionmentioning

confidence: 99%

See 2 more Smart Citations

Can Supernova Neutrino Nucleosynthesis Constrain Neutrino Oscillation Parameters?

Yoshida¹,

Kajino²,

Yokomakura³

et al. 2010

Proceedings of International Symposium on Nuclear Astrophysics - Nuclei in the Cosmos - IX — PoS(NIC-IX)

Self Cite

View full text Add to dashboard Cite

Recent neutrino experiment confirmed that neutrinos have finite masses and that neutrino oscillations occur. Supernova neutrinos also change their flavors propagating in the stellar material surrounding a proto-neutron star and, accordingly, change their spectral energy distributions. The nucleosynthesis of light elements such as 7 Li and 11 B is significantly enhanced through the ν-process in supernova explosions. Yields depend on the energy spectra of the neutrinos emitted from the proto-neutron star, so that neutrino oscillations could be crucial for the estimated yields of 7 Li, 11 B, and other isotopes produced in supernovae. We evaluate the 7 Li and 11 B yields in supernovae taking into account changes of the neutrino energy spectra due to flavor oscillations assuming large mixing angle solutions. We investigate their dependence on key parameters, such as mass hierarchies and the mixing angle θ 13 . In the case of a normal mass hierarchy and an adiabatic resonance of 13-mixing, the 7 Li yield is larger than that without neutrino oscillations by a factor of ∼ 2. For other parameter cases and for the 11 B yield in general, the enhancement is smaller. The increase of the 7 Li/ 11 B ratio is demonstrated for a normal mass hierarchy and a relatively large sin 2 2θ 13 , where 13-mixing resonance is adiabatic and sin 2 2θ 13 < 0.1. Thus, the detection of 7 Li/ 11 B enhancements in stars showing signs of supernova enrichment suggest a normal mass hierarchy and relatively large value of sin 2 2θ 13 .

show abstract

Massive Stars and Their Supernovae

Thielemann¹,

Diehl²,

Heger³

et al. 2018

Astrophysics With Radioactive Isotopes

View full text Add to dashboard Cite

Our understanding of stellar evolution and the final explosive endpoints such as supernovae or hypernovae or gamma-ray bursts relies on the combination of a) (magneto-)hydrodynamics b) engergy generation due to nuclear reactions accomanying composition changes c) radiation transport d) thermodynamic properties (such as the equation of state of stellar matter).Hydrodynamics is essentially embedded within the numerical schemes which implement the physics of processes (b) to (d). In early phases of stellar evolution, hydrodynamical processes can be approximated by a hydrostatic treatment. Nuclear energy production (b) includes all nuclear reactions triggered during stellar evolution and explosive end stages, also among unstable isotopes produced on the way. Radiation transport (c) covers atomic physics (e.g. opacities) for photon transport, but also nuclear physics and neutrino nucleon/nucleus interactions in late phases and core collapse. The thermodynamical treatment (d) addresses the mixture of ideal gases of photons, electrons/positrons and nuclei/ions. These are fermions and bosons, in dilute media or at high temperatures their energies can often be approximated by Maxwell-Boltzmann distributions. At very high densities, the nuclear equation of state is required to relate pressure and density. It exhibits a complex behavior, with transitions from individual nuclei to clusters of nucleons with a background neutron bath, homogeneous phases of nucleons, the emergence of hyperons and pions up to a possible hadron-quark phase transition.The detailed treatment of all these ingredients and their combined application is discussed in more depth in textbooks (Kippenhahn and Weigert, 1994; Maeder, /or the preceding Chapter (3), where the evolution of low and intermediate mass stars is addressed. That chapter also includes the stellar structure equations in spherical symmetry and a discussion of opacities for photon transport. Ch. 8 and 9 (tools for modeling objects and their processes) go into more detail with regard to modeling hydrodynamics, (convective) instabilities and energy transport as well as the energy generation due to nuclear reactions and the determination of the latter. Here we want to focus on the astrophysical aspects, i.e. a description of the evolution of massive stars and their endpoints with a special emphasis on the composition of their ejecta (in form of stellar winds during the evolution or of explosive ejecta). Low and intermediate mass stars end their evolution as AGB stars, finally blowing off a planetary nebula via wind losses and leaving a white dwarf with an unburned C and O composition. Massive stars evolve beyond this point and experience all stellar burning stages from H over He, C, Ne, O and Si-burning up to core collapse and explosive endstages. In this chapter we want to discuss the nucleosynthesis processes involved and the production of radioactive nuclei 5 in more detail. This includes all hydrostatic nuclear-burning stages experienced by massive stars, and explosive burning stages wh...

show abstract

Nucleosynthesis of Light Elements and Heavyr‐Process Elements through the ν‐Process in Supernova Explosions

Cited by 67 publications

References 59 publications

Metallicity-Dependent Galactic Isotopic Decomposition for Nucleosynthesis

Metallicity-Dependent Galactic Isotopic Decomposition for Nucleosynthesis

Can Supernova Neutrino Nucleosynthesis Constrain Neutrino Oscillation Parameters?

Massive Stars and Their Supernovae

Contact Info

Product

Resources

About