Neutrino processes in dense matter

Yueh, William R.; Buchler, J. R.

doi:10.1007/bf00684583

Cited by 32 publications

(17 citation statements)

References 6 publications

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“…c 5 . The terms I i (E, E , ω) are the phase-space integrals over the distribution functions as well as the separate 4-momenta terms of the squared and spin averaged matrix elements (expressed in terms of Fermi-Dirac integrals depending on the incoming E and the outgoing E neutrino energies, the electron mass m e , the temperature and the electron chemical potential μ e ), which are given in for example Yueh & Buchler (1976b), Schinder & Shapiro (1982) and Bruenn (1985). The weak interaction coefficients c A and c V are listed in Table 3 for the different reactions.…”

Section: Discussionmentioning

confidence: 99%

“…The neutrino pair-emissivity from electron-positron annihilation was calculated by Yueh & Buchler (1976a) and Yueh & Buchler (1976b). They explored the possibility of calculating the pairreaction rates in a similar way as neutrino-electron scattering (NES).…”

Section: Appendixmentioning

confidence: 99%

“…Following the argumentation and derivation by Yueh & Buchler (1976b), the emissivity for the traditional neutrino pair reaction (14) is given by the following expression…”

Section: Appendixmentioning

confidence: 99%

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The neutrino signal from protoneutron star accretion and black hole formation

Fischer

Whitehouse

Mezzacappa

et al. 2009

A&A

193

180

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Context. We discuss the formation of stellar mass black holes via protoneutron star (PNS) collapse. In the absence of an earlier explosion, the PNS collapses to a black hole due to the continued mass accretion onto the PNS. We present an analysis of the emitted neutrino spectra of all three flavors during the PNS contraction. Aims. Special attention is given to the physical conditions which depend on the input physics, e.g. the equation of state (EoS) and the progenitor model. Methods. The PNSs are modeled as the central object in core collapse simulations using general relativistic three-flavor Boltzmann neutrino transport in spherical symmetry. The simulations are launched from several massive progenitors of 40 M and 50 M . Results. We analyze the electron-neutrino luminosity dependencies and construct a simple approximation for the electron-neutrino luminosity, which depends only on the physical conditions at the electron-neutrinosphere. In addition, we analyze different (μ, τ)-neutrino pair-reactions separately and compare the differences during the post-bounce phases of failed core collapse supernova explosions of massive progenitors. We also investigate the connection between the increasing (μ, τ)-neutrino luminosity and the PNS contraction during the accretion phase before black hole formation. Conclusions. Comparing the different post bounce phases of the progenitor models under investigation, we find large differences in the emitted neutrino spectra. These differences and the analysis of the electron-neutrino luminosity indicate a strong progenitor model dependency of the emitted neutrino signal.

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Section: Discussionmentioning

confidence: 99%

Section: Appendixmentioning

confidence: 99%

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The neutrino signal from protoneutron star accretion and black hole formation

Fischer

Whitehouse

Mezzacappa

et al. 2009

A&A

193

180

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“…As A 2 _0, the curve describing the relation between U / a o and A/A J approaches the unit circle in the first quadrant of the plane (U/a o ' A/A J ), (~r = l-({Jr. (3.42) which isjust the linear dispersion relation of Jeans. 6 Thus, for every point (A2' AI) in the region D of Fig. 5(a), we can calculate a from (3.4) and the phase speed U / a o from (3.2).…”

Section: Derivation Of the Above Resultsmentioning

confidence: 99%

Nonlinear Waves in a Self‐Gravitating Medium

Yueh¹

1981

Stud Appl Math

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To investigate the effects of finite amplitudes on the behavior of waves in a self‐gravitating medium, exact solutions of nonlinear waves are obtained in a simple situation. The waves are traveling in the direction of the axis of rotation of a homogeneous and uniformly rotating self‐gravitating medium. The nonlinear wave profile and the dispersion relation are obtained and compared with Jeans's linear theory. It is found that the wavelength‐amplitude plane can be divided into three regions: (1) a region where the shock wave is expected to form, (2) a region where the neutral wave exists, and (3) a region where there is gravitational instability. In the third case, it is expected that the unstable wave will eventually evolve to a neutral wave with finite amplitude. Based on this result, speculations are made on the evolution of the unstable density wave in a galaxy. It is established that the propagation of the nonlinear wave in a self‐gravitating medium is always “subsonic,” just as in the linear theory. The difference is that the maximum ratio of the phase speed to the sound speed of the basic state is 1 − A2 for the isothermal case and (1 − A2)(γ + 1)/2 for the polytropic case instead of 1 for the linear case, where A2 is the dimensionless depth of the valley of the density profile, and γ is the polytropic index. It is also shown that no solitary wave can be found in a homogeneous self‐gravitating medium. Comparison is made with nonlinear waves in a homogeneous plasma.

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“…All the leptonic reactions (2)-(4) were calculated similar to ν e −e − scattering [22,23,25,26]. Figure 2 shows the (spectrally averaged) inverse mean free path of the relevant reactions for ν µ , including (1)-(3).…”

Section: Charged Current Reactions For Muon Neutrinosmentioning

confidence: 99%

CHARGED CURRENT INTERACTIONS OF numu NEUTRINOS IN SUPERNOVA

Lohs¹,

Martı́nez-Pinedo²,

Fischer³

2015

Proceedings of XIII Nuclei in the Cosmos — PoS(NIC XIII)

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Accurate neutrino transport is among the main ingredients to understand core-collapse supernovae and to perform numerical simulations of these events. The large amount and energy emitted in the form of neutrinos affects various distinct processes in supernovae. Neutrinos might trigger the explosion but they are also responsible for nucleosynthesis in neutrino driven wind. It is therefore necessary to study which neutrino reactions are relevant for which conditions. Here we explore the possible impact of additional reaction channels that are not included in current supernovae simulations. In particular we have investigated charged-current weak interactions for muon neutrinos and inverse neutron decay for electron antineutrinos at densities above 10 12 g cm −3 . It is shown that these reactions might affect the formation of neutrino spectra and neutrino signals from the interior of the protoneutron star. This could have further consequences especially for nucleosynthesis conditions in the neutrino driven wind.

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Neutrino processes in dense matter

Cited by 32 publications

References 6 publications

The neutrino signal from protoneutron star accretion and black hole formation

The neutrino signal from protoneutron star accretion and black hole formation

Nonlinear Waves in a Self‐Gravitating Medium

CHARGED CURRENT INTERACTIONS OF numu NEUTRINOS IN SUPERNOVA

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