Late-time behavior of fast neutrino oscillations

Bhattacharyya, Soumya; Dasgupta, Basudeb

doi:10.1103/physrevd.102.063018

Cited by 71 publications

(57 citation statements)

References 76 publications

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“…Eq. (2) also indicates a non-separable steady-state solution (non-collective) for P v (x) in position and velocity coordinates [4]. We numerically checked this via plotting the spatial variation of…”

Section: Resultsmentioning

confidence: 99%

Fast Neutrino Flavor Conversion at Late Time

Bhattacharyya¹

2021

Proceedings of 40th International Conference on High Energy Physics — PoS(ICHEP2020)

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Section: Resultsmentioning

confidence: 99%

Fast Neutrino Flavor Conversion at Late Time

Bhattacharyya¹

2021

Proceedings of 40th International Conference on High Energy Physics — PoS(ICHEP2020)

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“…Although the flavor evolution of this model can be inferred from the neutrino electronic lepton number (ELN) distribution and the dispersion relation (DR) when little flavor conversion has occurred [10][11][12], the few numerical explorations that have been made public so far seem to disagree qualitatively in the nonlinear regime. While our previous works show that fast oscillations can be coherent in space and time [13,14], the calculations from two other groups suggest that flavor depolarization should occur instead [15][16][17]. A recent study shows both the coherent flavor evolution in the short term and flavor depolarization in the long term when neutrinos are allowed to wrap around the periodic box [18].…”

Section: Introductionmentioning

confidence: 76%

Flavor isospin waves in one-dimensional axisymmetric neutrino gases

Duan,

Martin,

Omanakuttan

2021

Preprint

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Flavor oscillations can occur on very short spatial and temporal scales in the dense neutrino media in a core-collapse supernova (CCSN) or binary neutron star merger (BNSM) event. Although the dispersion relations (DRs) of the fast neutrino oscillations can be obtained by linearizing the equations of motion (EoM) before the emergence of any significant flavor conversion, one largely depends on numerical calculations to understand this interesting phenomenon in the nonlinear regime. In this work we demonstrate that there exist nontrivial solutions to the flavor EoM that govern the fast oscillations in one-dimensional axisymmetric neutrino gases. These solutions represent a coherent flavor isospin wave similar to the magnetic spin wave in a lattice of magnetic dipoles. We also compute the DRs of such waves in some example cases which are closely related to the DRs of the fast neutrino oscillations obtained in the linear regime. This result sheds new light on the long-term behavior of fast neutrino oscillations which can have various implications for the CCSN and BNSM events.

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“…The majority of the simulations so far assume homogeneity ("one-zone" models) and are discretized in only angle (or angular moments) and time. These simulations have demonstrated a consistency between linear stability analysis and direct evolution of the nonlinear equations [65][66][67][68] and have shed some insight into the late-time angular turbulence and kinematic decoherence [69][70][71]. Other simulations of the FFI have included inhomogeneity [72,73], a simplified treatment of collisional processes [74], or both [50].…”

Section: Introductionmentioning

confidence: 77%

Particle-in-cell Simulation of the Neutrino Fast Flavor Instability

Richers,

Willcox,

Ford

et al. 2021

Preprint

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Neutrinos drive core-collapse supernovae, launch outflows from neutron star merger accretion disks, and set the ratio of protons to neutrons in ejecta from both systems that generate heavy elements in the universe. Neutrinos of different flavors interact with matter differently, and much recent work has suggested that fast flavor instabilities are likely ubiquitous in both systems, but the final flavor content after the instability saturates has not been well understood. In this work we present particle-in-cell calculations which follow the evolution of all flavors of neutrinos and antineutrinos through saturation and kinematic decoherence. We conduct one-dimensional threeflavor simulations of neutrino quantum kinetics to demonstrate the outcome of this instability in a few example cases. We demonstrate the growth of both axially symmetric and asymmetric modes whose wavelength and growth rate match predictions from linear stability analysis. Finally, we vary the number density, flux magnitude, and flux direction of the neutrinos and antineutrinos and demonstrate that these factors modify both the growth rate and post-saturation neutrino flavor abundances. Weak electron lepton number (ELN) crossings in these simulations produce both slow growth of the instability and little difference between the flavor abundances in the initial and final states. In all of these calculations the same number of neutrinos and antineutrinos change flavor, making the least abundant between them the limiting factor for post-saturation flavor change. Many more simulations and multi-dimensional simulations are needed to fully probe the parameter space of the initial conditions.

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Late-time behavior of fast neutrino oscillations

Cited by 71 publications

References 76 publications

Fast Neutrino Flavor Conversion at Late Time

Fast Neutrino Flavor Conversion at Late Time

Flavor isospin waves in one-dimensional axisymmetric neutrino gases

Particle-in-cell Simulation of the Neutrino Fast Flavor Instability

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