RECORD
Spread Complexity of High Energy Neutrino Propagation over Astrophysical Distances
High Energy Physics - Phenomenology · Submitted 11 Jun 2024
abstract compiled · 2026-09-23 · no language-model review
The authors' main claim Our findings indicate that our proposal might favor an initial ratio of fluxes as $\phi_{\nu_e}^0: \phi_{\nu_\mu}^0: \phi_{\nu_\tau}^0 = 1:0:0$ over a more generally expected ratio of $1:2:0$, when the IceCube neutrino observatory achieves its projected sensitivity to discriminate between flavors.
The compiled record
The paper's own sentences, arranged. Each label is drawn from a closed vocabulary; the number beside it is the probability the classifier gave that label. Numbers in the tables are the authors', checked by code. No sentence in this record was written by a model.
Open the compiled record
The abstract, sentence by sentence
Spread complexity measures the minimized spread of quantum states over all choices of basis. It generalizes Krylov operator complexity to quantum states under continuous Hamiltonian evolution. In this paper, we study spread complexity in the context of high-energy astrophysical neutrinos and propose a new flavor ratio based on complexity. Our findings indicate that our proposal might favor an initial ratio of fluxes as $\phi_{\nu_e}^0: \phi_{\nu_\mu}^0: \phi_{\nu_\tau}^0 = 1:0:0$ over a more generally expected ratio of $1:2:0$, when the IceCube neutrino observatory achieves its projected sensitivity to discriminate between flavors. Additionally, complexity-based definitions of flavor ratios exhibit a slight but nonzero sensitivity to the neutrino mass ordering, which traditional flavor ratios cannot capture.
background contribution method result interpretation main claim
| # | sentence | role | the authors' own work | states the main conclusion | strength |
|---|---|---|---|---|---|
| s0 | Spread complexity measures the minimized spread of quantum states over all choices of basis. | background 0.99 | 0.06 | 0.02 | asserted 1.00 |
| s1 | It generalizes Krylov operator complexity to quantum states under continuous Hamiltonian evolution. | background 1.00 | 0.09 | 0.02 | asserted 1.00 |
| s2 | In this paper, we study spread complexity in the context of high-energy astrophysical neutrinos and propose a new flavor ratio based on complexity. | contribution 1.00 | 0.82 | 0.08 | asserted 0.97 |
| s3 | Our findings indicate that our proposal might favor an initial ratio of fluxes as $\phi_{\nu_e}^0: \phi_{\nu_\mu}^0: \phi_{\nu_\tau}^0 = 1:0:0$ over a more generally expected ratio of $1:2:0$, when the IceCube neutrino observatory achieves its projected sensitivity to discriminate between flavors. | result 0.98 | 0.93 | 0.70 | hedged possibility 0.84 |
| s4 | Additionally, complexity-based definitions of flavor ratios exhibit a slight but nonzero sensitivity to the neutrino mass ordering, which traditional flavor ratios cannot capture. | result 0.99 | 0.88 | 0.11 | asserted 0.99 |
What was examined, and what was not
- arXiv listing abstract v2
- full text
- figures and tables
- references and citing sentences
- relations to other papers
- P abstract
- S sections
- T body sentences
- C citations
- R cross-paper relations
The paper
Original abstract
Spread complexity measures the minimized spread of quantum states over all choices of basis. It generalizes Krylov operator complexity to quantum states under continuous Hamiltonian evolution. In this paper, we study spread complexity in the context of high-energy astrophysical neutrinos and propose a new flavor ratio based on complexity. Our findings indicate that our proposal might favor an initial ratio of fluxes as $\phi_{\nu_e}^0: \phi_{\nu_\mu}^0: \phi_{\nu_\tau}^0 = 1:0:0$ over a more generally expected ratio of $1:2:0$, when the IceCube neutrino observatory achieves its projected sensitivity to discriminate between flavors. Additionally, complexity-based definitions of flavor ratios exhibit a slight but nonzero sensitivity to the neutrino mass ordering, which traditional flavor ratios cannot capture.
Human review
How the literature uses it
2 arXiv papers cite this in 2 sentences
Papers citing it
Cites it as background 2 papers
-
While Krylov complexity has been extensively studied in diverse systems [ref] , the formalism relies on the existence of a time-independent Hamiltonian to generate time evolution.
Quantum chaos and complexity from string scattering amplitudes · Introduction · 0.91
-
From experiments at the Large Hadron Collider (LHC) [ref] to astroparticle observations [ref] and neutrino phenomenology [ref] , the study of quantum correlations, including entanglement, has demonstrated significant potential, opening new avenues for exploration.
Quantum Information as a New Lens for Precision Neutrino Physics · Introduction · 0.90
What it cites · 53 sentences without a confident label
Uses data or values from 1 paper
-
However, the best-fit point (see Fig. [ref]) gives a ratio of $0.20:0.39:0.42$ [ref] , which corresponds to an initial flavor ratio close to $0:1:0$ with the traditional probability-based flavor ratio expectation.
2011.03561 · Results · 0.96
Cites as background 45 papers
-
The initial $ν_τ$ flavor is supposed to be zero as the neutrino production mechanism in these high energy astrophysical objects like blazars or AGNs are considered to be either neutron beta decay, $n→p+e^-+ν̅_e$, which induces initial flavor ratio of $ϕ_e^0:ϕ_μ^0:ϕ_τ^0 = 1:0:0$, or pion decay created by interactions of shock-accelerated protons/ions with surrounding radiation (p-$γ$) or gas (p-p), $π^+→e^+ + ν_e + ν̅_μ+ ν_μ$, with initial flavor ratio of $1:2:0$, see, e.g., Refs. [ref] Astrophysical environment effects such as efficient synchrotron cooling of secondary muons in strong magnetic fields can prompt the initial ratio to be 0:1:0 (muon-damped) at higher energies, however, for lower energy of muons the flavor ratio of 1:1:0 is highly probable, see e.g., Refs. [ref] .
Describing the Observed Cosmic Neutrinos by Interactions of Nuclei with Matter · Astrophysical neutrino oscillations and flavor ratios · 0.86
-
The initial $ν_τ$ flavor is supposed to be zero as the neutrino production mechanism in these high energy astrophysical objects like blazars or AGNs are considered to be either neutron beta decay, $n→p+e^-+ν̅_e$, which induces initial flavor ratio of $ϕ_e^0:ϕ_μ^0:ϕ_τ^0 = 1:0:0$, or pion decay created by interactions of shock-accelerated protons/ions with surrounding radiation (p-$γ$) or gas (p-p), $π^+→e^+ + ν_e + ν̅_μ+ ν_μ$, with initial flavor ratio of $1:2:0$, see, e.g., Refs. [ref] Astrophysical environment effects such as efficient synchrotron cooling of secondary muons in strong magnetic fields can prompt the initial ratio to be 0:1:0 (muon-damped) at higher energies, however, for lower energy of muons the flavor ratio of 1:1:0 is highly probable, see e.g., Refs. [ref] .
High energy neutrino yields from astrophysical sources I: Weakly magnetized sources · Astrophysical neutrino oscillations and flavor ratios · 0.86
-
The initial $ν_τ$ flavor is supposed to be zero as the neutrino production mechanism in these high energy astrophysical objects like blazars or AGNs are considered to be either neutron beta decay, $n→p+e^-+ν̅_e$, which induces initial flavor ratio of $ϕ_e^0:ϕ_μ^0:ϕ_τ^0 = 1:0:0$, or pion decay created by interactions of shock-accelerated protons/ions with surrounding radiation (p-$γ$) or gas (p-p), $π^+→e^+ + ν_e + ν̅_μ+ ν_μ$, with initial flavor ratio of $1:2:0$, see, e.g., Refs. [ref] Astrophysical environment effects such as efficient synchrotron cooling of secondary muons in strong magnetic fields can prompt the initial ratio to be 0:1:0 (muon-damped) at higher energies, however, for lower energy of muons the flavor ratio of 1:1:0 is highly probable, see e.g., Refs. [ref] .
High energy neutrino yields from astrophysical sources II: Magnetized sources · Astrophysical neutrino oscillations and flavor ratios · 0.86
Discussion
Know something about this paper? Leave a comment, or highlight any passage above to comment on it.