Instabilities and propagation of neutrino magnetohydrodynamic waves in arbitrary direction

Haas, Fernando; Pascoal, Kellen Alves

doi:10.1063/1.4997187

Cited by 8 publications

(23 citation statements)

References 22 publications

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“…It was assumed that ω ω pi = Z n 0 e 2 /(m i ε 0 ) and E 0 = E e0 ≈ E μ0 . By inspection, it is not surprising that the dispersion relation, (14), is formally identical to the result in [8] (with a new expression for the ion-acoustic speed), since in the linearization procedure one has γ ≈ 1 due to the absence of relativistic streaming electrons.…”

Section: Linear Wavesmentioning

confidence: 81%

“…In addition, magnetized plasmas can be treated by simply including the magnetic force on electrons and ions [15]. In the case of electromagnetic waves, also the full set of Maxwell equations would be necessary [13,14]. To close the system, one needs the equations for the twoflavor oscillations.…”

Section: Basic Modelmentioning

confidence: 99%

“…Previously, neutrino oscillations in nonrelativistic plasmas have also been analyzed in [11] and [12], taking into account the collisional damping of ion-acoustic waves. In addition, neutrino-magnetohydrodynamic modes [13,14] and neutrinomodified wave propagation in strongly magnetized plasma * fernando.haas@ufrgs.br [15] have been considered, without the inclusion of flavor oscillations, degeneracy, or relativistic effects.…”

Section: Introductionmentioning

confidence: 99%

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Neutrino oscillations and instabilities in degenerate relativistic astrophysical plasmas

Haas

2019

Phys. Rev. E

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We set up a proposal to extend significantly recent works on neutrino-plasma interaction, allowing the possibility of deep degenerate and relativistic electrons, which are often present in compact stars such as high-density white dwarfs. The methodology involves the covariant hydrodynamic formulation of ultradense plasmas. We propose the generalization of previous studies, on the interaction between ion-acoustic waves and resonant neutrino flavor oscillations in a mixed neutrino beam, admitting degenerate and relativistic electron populations. Destabilization of the ion acoustic wave has higher growth rates, thanks to the very high densities present in plasmas under these extreme conditions. We take into account applications to white dwarf stars in the process of collapsing, producing type II supernovas.

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Section: Linear Wavesmentioning

confidence: 81%

Section: Basic Modelmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Neutrino oscillations and instabilities in degenerate relativistic astrophysical plasmas

Haas

2019

Phys. Rev. E

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“…It was found out that NMHD proved that the destabilization of the magnetosonic wave by neutrino beam could be one of the reasons behind the supernova explosion. Similarly the neutrino beam instabilities of magnetosonic waves in arbitrary direction for fast and slow waves are also investigated by taking into account the weak Fermi force due to neutrinos coupling with MHD plasmas [18]. The maximum growth rate of slow and fast magnetosonic waves comes out to be of same order at different wave propagation angles.…”

Section: Introductionmentioning

confidence: 99%

“…In the present work, the growth rate of neutrino-driven instability in the fast and slow magnetosonic waves in dense plasmas (but in classical regime) is studied using the multi-fluid model containing electron-ion plasma and neutrino beam with the inclusion of the ions and neutrals (atoms) collisions in the model. The effect of ionneutral collisions on the growth rate of neutrino beam instability on magnetosonic waves has not been investigated in earlier published work [17,18] and references therein. The detailed investigation of the growth rate of neutrino beam instability for magnetosonic waves in plasmas with variations in magnetic field angle, neutrino beam density, neutrino beam energy and magnetic field intensity is also presented.…”

Section: Introductionmentioning

confidence: 99%

Neutrino beam driven instability of magnetosonic waves in the presence of oblique magnetic field and ion-neutral collisional effect in plasmas

Aftab¹,

Hussain²,

Mahmood³

et al. 2022

Phys. Scr.

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The neutrino beam driven instability of fast and slow magnetosonic waves with oblique applied magnetic field in multi-component ion, electron, and neutrino beam plasma is studied. The dissipation effects of ion-neutral collisions are also included in the model. The neutrino and electron interactions through electro-weak force are included. It is found that the dissipation of ion collisions has significant effect on the phase velocity of the wave propagation and growth rate of the neutrino beam driven instability. The analytical expression of the growth rate of the fast and slow magnetosonic waves instability is found under the weak neutrino beam approximation and in the absence of ions and neutrals (atoms) collision effect. The numerical illustration of growth rates of the fast and slow magnetosonic waves are also presented with variations of magnetic field angle, neutrino beam energy, neutrino beam density, magnetic field intensity. It is found that the growth rate of the fast magnetosonic wave is maximum in case of the perpendicular directed magnetic field to the direction of wave propagation, while growth rate of slow magnetosonic wave is minimum in that case. It is also noticed that growth rate of fast magnetosonic wave comes out to be larger (of the order tens) than the slow magnetosonic wave case, which is quite different from earlier published results of Type II core-collapse supernova.

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Influence of neutrino beam on the Jeans instability in a magnetized quantum plasma

Prajapati

2017

Physics of Plasmas

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The influence of propagation dynamics of intense neutrino beams on the hydrodynamic Jeans instability in a magnetized quantum plasma is investigated. The dynamics of a self-gravitating, magnetized electron-ion quantum plasma weakly interacting with neutrinos are considered in a neutrino magnetohydrodynamic model. The modified dispersion relations of Jeans instability and fast neutrino-driven short wavelength instability are established using a linear perturbation method. In oblique propagation, the Jeans instability condition is modified due to the presence of neutrino beam effects, whereas no effect was observed in parallel and perpendicular propagations. The neutrino beam density stabilizes, while the free energy of the neutrino beam destabilizes the growth rate of Jeans instability. The estimated Jeans time scale is comparable to the time scale of supernova explosion. The time scale of neutrino beam instability is much shorter than the Jeans time scale which results in faster neutrino mixing in the gravitational collapse of the system. The consequences of neutrino beam interactions with a magnetized, self-gravitating quantum plasma have been addressed in astrophysical environments.

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Instabilities and propagation of neutrino magnetohydrodynamic waves in arbitrary direction

Abstract: In a previous work [16], a new model was introduced, taking into account the role of the Fermi weak force due to neutrinos coupled to magnetohydrodynamic plasmas. The resulting neutrino-

Cited by 8 publications

References 22 publications

Neutrino oscillations and instabilities in degenerate relativistic astrophysical plasmas

Neutrino oscillations and instabilities in degenerate relativistic astrophysical plasmas

Neutrino beam driven instability of magnetosonic waves in the presence of oblique magnetic field and ion-neutral collisional effect in plasmas

Influence of neutrino beam on the Jeans instability in a magnetized quantum plasma

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