Supernovae, neutrinos, and nucleosynthesis

Fröhlich, C.

doi:10.1088/0954-3899/41/4/044003

Cited by 12 publications

(16 citation statements)

References 106 publications

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“…While rigorous proofs for triviality exist for d > 4 [10], strong evidence for triviality in d = 4 has been collected by lattice simulations [11][12][13][14][15][16][17] as well as by functional renormalization group (RG) studies [18]. Similar conclusions appear to hold for QED [19,20].…”

Section: Introductionmentioning

confidence: 92%

Non-Abelian Higgs models: Paving the way for asymptotic freedom

Gies¹,

Zambelli²

2017

Phys. Rev. D

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Asymptotically free renormalization group trajectories can be constructed in nonabelian Higgs models with the aid of generalized boundary conditions imposed on the renormalized action. We detail this construction within the languages of simple low-order perturbation theory, effective field theory, as well as modern functional renormalization group equations. We construct a family of explicit scaling solutions using a controlled weak-coupling expansion in the ultraviolet, and obtain a standard Wilsonian RG relevance classification of perturbations about scaling solutions. We obtain global information about the quasi-fixed function for the scalar potential by means of analytic asymptotic expansions and numerical shooting methods. Further analytical evidence for such asymptotically free theories is provided in the large-N limit. We estimate the long-range properties of these theories, and identify initial/boundary conditions giving rise to a conventional Higgs phase.

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Section: Introductionmentioning

confidence: 92%

Non-Abelian Higgs models: Paving the way for asymptotic freedom

Gies¹,

Zambelli²

2017

Phys. Rev. D

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“…Explosion energies of this magnitude are beyond the reach of the neutrino-driven mechanism, and as such, we also neglect neutrino transport in our models. We assume that whatever the hypernova mechanism is in reality, ejecta are immediately heated and ejected by a powerful shock, and not exposed to any significant neutrino flux from the cooling neutron star as in the neutrino-driven mechanism, which would otherwise affect nucleosynthesis (e.g., Buras et al 2006;Marek & Janka 2009;Müller et al 2012a;Fröhlich 2014). Although there may be another ejecta component that is more strongly neutrino-processed or has undergone stronger deleptonisation (e.g., from a proto-neutron star or collapsar disk wind), nucleosynthesis by explosive burning will always contribute and can justifiably be investigated using our piston-driven models.…”

Section: Initial Models and Proceduresmentioning

confidence: 99%

Nucleosynthesis in Primordial Hypernovae

Grimmett

Heger

Karakas

et al. 2018

Monthly Notices of the Royal Astronomical Society

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We investigate the relationship between explosion energy and nucleosynthesis in Population III supernovae and provide nucleosynthetic results for the explosions of stars with progenitor masses of 15 M , 20 M , 30 M , 40 M , 60 M , and 80 M , and explosion energies between approximately 10 50 erg and 10 53 erg. We find that the typical abundance pattern observed in metal-poor stars are best matched by supernovae with progenitor mass in the range 15 M -30 M , and explosion energy of ∼ (5 − 10) × 10 51 erg. In these models, a reverse shock caused by jumps in density between shells of different composition serves to decrease synthesis of chromium and manganese, which is favourable to matching the observed abundances in metal-poor stars. Spherically symmetric explosions of our models with progenitor mass ≥ 40 M do not provide yields that are compatible with the iron-peak abundances that are typically observed in metal-poor stars, however, by approximating the yields that we might expect from these models in highly aspherical explosions, we find indications that explosions of stars 40 M -80 M with bipolar jets may be good candidates for the enrichment sources of metal-poor stars with enhanced carbon abundances.

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“…This is in contrast to the situation of the purescalar models which are now widely believed to be trivial (see, e.g., Refs. [17,18]). In our previous attempt at addressing the issue of the triviality in the Higgs-Yukawa model, as reported in Ref.…”

Section: Finite-size Scaling For the Higgs-yukawa Model Near The Gausmentioning

confidence: 99%

Higgs-Yukawa model on the lattice

et al. 2018

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Abstract. We present results from two projects on lattice calculations for the HiggsYukawa model. First we report progress on the search of first-order thermal phase transitions in the presence of a dimension-six operator, with the choices of bare couplings that lead to viable phenomenological predictions. In this project the simulations are performed using overlap fermions. Secondly, our study for applying finite-size scaling techniques near the Gaussian fixed point of the Higgs-Yukawa model is presented. We discuss the analytical formulae for the Higgs Yukawa model and show results for a first numerical study in the pure O(4) scalar sector of the theory.

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Supernovae, neutrinos, and nucleosynthesis

Cited by 12 publications

References 106 publications

Non-Abelian Higgs models: Paving the way for asymptotic freedom

Non-Abelian Higgs models: Paving the way for asymptotic freedom

Nucleosynthesis in Primordial Hypernovae

Higgs-Yukawa model on the lattice

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