Neutrino Driven Streaming Instabilities in a Dense Plasma

Silva, L. O.; Bingham, R.; Dawson, J. M.; Mendonça, J. T.; Shukła, P. K.

doi:10.1103/physrevlett.83.2703

Cited by 108 publications

(141 citation statements)

References 19 publications

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“…Hence, the above growth rate estimate is always defined for the relevant scenarios. Also observe the growth rate is ∝ G 2/3 F which is the same estimate as in [8] for a weak neutrino beam. Revealing insights can be obtained rewriting the dispersion relation in terms of a characteristic function F (ω) as…”

Section: Incoherent Neutrino Beamsupporting

confidence: 66%

“…(5) depends on the energy of the neutrino beam, and is well defined for a (nearly mono-energetic) beam, such that E e = E µ = E 0 . The momentum equations in (8) show that, in the presence of plasma perturbations E = 0 and B = 0, the quantities v e and v µ are not necessarily identical.…”

Section: Fluid Descriptionmentioning

confidence: 99%

“…Finally, the neutrino oscillations are influenced by the plasma in two ways: due to the coupling with n in ζ in Eq. (7) and due to the role of the electromagnetic field in the electron neutrino momentum equation (8). In the following, illustrative examples of applications are provided.…”

Section: Fluid Descriptionmentioning

confidence: 99%

“…Second, they create an induced neutrino charge [6,7], which can lead to collective plasma oscillations and significantly increase the collision cross sections. The energy transfer between a neutrino beam and plasma wave is mediated by the neutrino Landau damping [8]. The individual flavor processes are important to understand the solar neutrino deficit, while the collective plasma effects could play a major role in supernova explosions [9].…”

Section: Introductionmentioning

confidence: 99%

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Influence of flavor oscillations on neutrino beam instabilities

2014

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We consider the collective neutrino plasma interactions, and study the electron plasma instabilities produced by a nearly mono-energetic neutrino beam in a plasma. We describe the mutual influence of neutrino flavor oscillations and electron plasma waves. We show that the neutrino flavor oscillations are not only perturbed by electron plasmas waves, but also contribute to the dispersion relation and the growth rates of neutrino beam instabilities.

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Section: Incoherent Neutrino Beamsupporting

confidence: 66%

Section: Fluid Descriptionmentioning

confidence: 99%

Section: Fluid Descriptionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Influence of flavor oscillations on neutrino beam instabilities

2014

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“…It is well known that neutrinos interact with the background dense plasma through the weak nuclear force [1][2][3][4][5][6]. The dispersion relation for neutrino oscillations in plasmas is…”

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confidence: 99%

Amplification of neutrino oscillations by a density ripple in dense plasmas

Shukła

2011

J. Plasma Phys.

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Abstract. It is shown that a pre-existing electron density ripple in a dense plasma can excite electron neutrino oscillations. For our purposes, we use the dispersion relation for neutrino oscillations and derive the Mathieu equation for the propagation of neutrino oscillations in the presence of a spatially oscillating electron density ripple. The Mathieu equation predicts instability of neutrino oscillations. The criterion under which instability occurs is presented. Analytical expressions for the neutrino oscillation frequency and the growth rate are obtained. The possible relevance of our investigation to non-thermal neutrino oscillations in dense plasma environments (e.g. the supernovae, the core of white dwarf stars etc.) is briefly mentioned.Neutrinos, which are the least massive subatomic ghostly elementary particles in the set of building blocks of nature, were produced in the Big-Bang, which began the universe, and are emitted by the Sun and all other stars (e.g. neutron stars, white dwarf stars, magnetars etc.) These are also produced in violent astrophysical events in cosmos, e.g. explosions of supernovae, which occur when an old massive star collapses after running out of nuclear fuel. During the collapse, the star literally becomes a neutron star as neutrinos totally dominate in numbers of particles for a few seconds and carry off most of the energy from the implosion, more energy than radiated during the entire life of the star. For example, the neutrino flash was actually observed in Supernova 1987A. Neutrinos are also created when cosmic rays, fast moving particles from space, bombard the Earth's atmosphere producing cascades of secondary particles, which rain down on us. There are three different kinds, or 'flavors', as they are called, of neutrinos: electron, muon and tau neutrinos. There are also three anti-neutrinos of the same flavors. The neutrinos get their names from their charged lepton brethren, the electron, muon and tau, with masses of 0.511 MeV, 106 MeV and 1777 Mev, respectively. The three species of neutrinos at https://www.cambridge.org/core/terms. https://doi

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Magnetic Helicity in Rotating Neutron Stars

Dvornikov

2023

Geophysical Monograph Series

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Neutrino Driven Streaming Instabilities in a Dense Plasma

Cited by 108 publications

References 19 publications

Influence of flavor oscillations on neutrino beam instabilities

Influence of flavor oscillations on neutrino beam instabilities

Amplification of neutrino oscillations by a density ripple in dense plasmas

Magnetic Helicity in Rotating Neutron Stars

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