The role of medium modifications for neutrino-pair processes from nucleon-nucleon bremsstrahlung

Fischer, Tobias

doi:10.1051/0004-6361/201628991

Cited by 54 publications

(51 citation statements)

References 81 publications

(93 reference statements)

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“…The matter density and temperature of our model shown in Fig. 2 and 3 correspond to the simulation of the protoneutron star deleptonization of [55] without considering axions. The left panels show the radial behavior of temperature and density at different post-bounce times t pb , while the right panels present contours of T and ρ in the t pb and radial coordinate r plane.…”

Section: Impact Of the Different Corrections Sn Reference Modelmentioning

confidence: 96%

Improved axion emissivity from a supernova via nucleon-nucleon bremsstrahlung

Carenza

Fischer

Giannotti

et al. 2019

J. Cosmol. Astropart. Phys.

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The most efficient axion production mechanism in a supernova (SN) core is the nucleon-nucleon bremsstrahlung. This process has been often modeled at the level of the vacuum one-pion exchange (OPE) approximation. Starting from this recipe, we revise the calculation including systematically different effects, namely a non-vanishing mass for the exchanged pion, the contribution from the two-pions exchange, effective in-medium nucleon masses and multiple nucleon scatterings. Moreover, we allow for an arbitrary degree of nucleon degeneracy. A self consistent treatment of the axion emission rate including all these effects is currently missing. The aim of this work is to provide such an analysis. We find that the axion emissivity is reduced by over an order of magnitude with respect to the basic OPE calculation, after all these effects are accounted for. The implications for the axion mass bound and the impact for the next generation experimental axion searches will be discussed.

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Section: Impact Of the Different Corrections Sn Reference Modelmentioning

confidence: 96%

Improved axion emissivity from a supernova via nucleon-nucleon bremsstrahlung

Carenza

Fischer

Giannotti

et al. 2019

J. Cosmol. Astropart. Phys.

Self Cite

202

255

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“…The radial temperature profile of our SN model, at three different post-bounce times t pb , shown in Fig. 1, corresponds to the simulation of the protoneutron star deleptonization of [27]. We can see that the temperature T presents a peak of ∼ 40 MeV at r 10 km.…”

Section: Sn Reference Modelmentioning

confidence: 79%

Heavy sterile neutrino emission in core-collapse supernovae: constraints and signatures

Mastrototaro¹,

Mirizzi

Serpico

et al. 2020

J. Cosmol. Astropart. Phys.

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Heavy sterile neutrinos with masses O(100) MeV mixing with active neutrinos can be produced in the core of a collapsing supernova (SN). In order to avoid an excessive energy loss, shortening the observed duration of the SN 1987A neutrino burst, we show that the active-sterile neutrino mixing angle should satisfy sin 2 θ 5 × 10 −7 . For a mixing with tau flavour, this bound is much stronger than the ones from laboratory searches. Moreover, we show that in the viable parameter space the decay of such "heavy" sterile neutrinos in the SN envelope would lead to a very energetic flux of daughter active neutrinos; if not too far below current limits, this would be detectable in large underground neutrino observatories, like Super-Kamiokande, as a (slightly time-delayed) high-energy bump in the spectrum of a forthcoming Galactic SN event.

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“…In set6a, quenching of the axial-vector coupling constant at high densities (Carter & Prakash 2002) (e.g., Equation (A.9) in Buras et al (2006b)) is included but using more recent fitting formula (e.g., Equation (8) in Fischer (2016)). In set6b, we employ the formulas suggested by Horowitz et al (2017) for the neutral-current axial response that accounts for virial effects at low density and many-body correlations at high densities ).…”

Section: Neutrino Opacitiesmentioning

confidence: 99%

“…The comparison plots between set4b (not shown) and set1 are almost completely overlayed (like in the middle left panel of Figure 12 or in the bottom right panel of Figure 8). It was shown (e.g., Fischer (2016) and Bartl et al (2016)) that the medium suppression of Bremsstrahlung affects the neutrino properties only clearly after the onset of an explosion and the following PNS cooling phase. In this respect, our results showing a negligle impact in the pre-explosion phase are in line with the literature.…”

Section: Mean-field Modifications (Set4a and Set4b)mentioning

confidence: 99%

“…In the original IDSA scheme ), a base-line set of neutrino opacities (Bruenn 1985) (often referred to as the Bruenn rate) is used. Following the implementation schemes of microphysical update in the literature (e.g., Buras et al (2006b); Fischer et al (2009);Fischer (2016)), we 1 In order to clearly see the effect, Melson et al (2015a) chose a relatively high strangeness contribution (g s a = −0.2) to the axial vector coupling constant (ga ≈ 1.26) compared to the constraint (g s a −0.1) proposed by Hobbs et al (2016). study how individual update in the neutrino opacity leads to differences from the base-line run with the Bruenn rate.…”

Section: Introductionmentioning

confidence: 99%

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Impact of Neutrino Opacities on Core-collapse Supernova Simulations

Kotake

Takiwaki

Fischer

et al. 2018

ApJ

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Accurate description of neutrino opacities is central both to the core-collapse supernova (CCSN) phenomenon and to the validity of the explosion mechanism itself. In this work, we study in a systematic fashion the role of a variety of well-selected neutrino opacities in CCSN simulations where multi-energy, three-flavor neutrino transport is solved by the isotropic diffusion source approximation (IDSA) scheme. To verify our code, we first present results from one-dimensional (1D) simulations following corecollapse, bounce, and up to ∼ 250 ms postbounce of a 15M ⊙ star using a standard set of neutrino opacities by Bruenn (1985). Detailed comparison with published results supports the reliability of our three-flavor IDSA scheme using the standard opacity set. We then investigate in 1D simulations how the individual opacity update leads to the difference from the base-line run with the standard opacity set. By making a detailed comparison with previous work, we check the validity of our implementation of each update in a step-by-step manner. Individual neutrino opacities with the largest impact on the overall evolution in 1D simulations are selected for a systematic comparison in our two-dimensional (2D) simulations. Special emphasis is devoted to the criterion of explodability in the 2D models. We discuss the implications of these results as well as the limitations and requirements for future towards more elaborate CCSN modeling.

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The role of medium modifications for neutrino-pair processes from nucleon-nucleon bremsstrahlung

Cited by 54 publications

References 81 publications

Improved axion emissivity from a supernova via nucleon-nucleon bremsstrahlung

Improved axion emissivity from a supernova via nucleon-nucleon bremsstrahlung

Heavy sterile neutrino emission in core-collapse supernovae: constraints and signatures

Impact of Neutrino Opacities on Core-collapse Supernova Simulations

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