Astrophysics · arXiv:astro-ph/0404099 v1 · submitted 5 Apr 2004
Fluid Stability Below the Neutrinospheres of Supernova Progenitors and the Dominant Role of Lepto-Entropy Fingers
The paper says
“An important consequence of this is the presence of a doubly diffusive instability, which we refer to as “lepto-entropy fingers,” in an extensive region below the neutrinosphere where the lepton number, Yℓ, is small.”
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Abstract
We have developed a formalism for analyzing the stability of a fluid in the presence of neutrinos of all flavors and in the presence of a gravitational field. When applied to an extensive two-dimensional grid of core radii and fluid element sizes for each of several time slices of a number of proto-supernovae, we find no evidence for the neutron finger instability as described by the Livermore group. We find, instead, that the rate of lepton equilibration always exceeds that of thermal equilibration. Furthermore, we find that thermal diffusion driven by a lepton fraction difference and lepton diffusion driven by an entropy difference are both nonzero and that the first of these tends to be large in magnitude. An important consequence of this is the presence of a doubly diffusive instability, which we refer to as “lepto-entropy fingers,” in an extensive region below the neutrinosphere where the lepton number, Yℓ, is small. This instability is driven by a mechanism very different from that giving rise to neutron fingers, and may play an important role in enhancing the neutrino emission. Deep in the core where the entropy is low and the lepton number higher, our analysis indicates a region unstable to another instability which we refer to as “lepto-entropy semiconvection.” These instabilities, particularly lepto-entropy fingers, may have already been seen in some multi-dimensional core collapse simulations described in the literature.
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abstract compiled · 2026-09-23 · no language-model review
How the main claim is stated: asserted 1.00
What the abstract itself states, as probabilities: claims first 0.06 · states limitation 0.18 · human participants 0.01 · controlled comparison 0.10 · randomized assignment 0.01 · states quantitative result 0.10 · compares with prior results 0.95 · mentions code or data availability 0.02
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This table labels the abstract only (arXiv listing abstract v1). The number is the probability the classifier gave the label.
| Sentence | Role | The authors' own work | States the main conclusion | Strength |
|---|---|---|---|---|
| We have developed a formalism for analyzing the stability of a fluid in the presence of neutrinos of all flavors and in the presence of a gravitational field. | contribution 0.64 | 0.95 | 0.03 | asserted 1.00 |
| When applied to an extensive two-dimensional grid of core radii and fluid element sizes for each of several time slices of a number of proto-supernovae, we find no evidence for the neutron finger instability as described by the Livermore group. | result 0.98 | 0.96 | 0.18 | asserted 1.00 |
| We find, instead, that the rate of lepton equilibration always exceeds that of thermal equilibration. | result 1.00 | 0.96 | 0.14 | asserted 1.00 |
| Furthermore, we find that thermal diffusion driven by a lepton fraction difference and lepton diffusion driven by an entropy difference are both nonzero and that the first of these tends to be large in magnitude. | result 1.00 | 0.94 | 0.08 | asserted 1.00 |
| An important consequence of this is the presence of a doubly diffusive instability, which we refer to as ``lepto-entropy fingers,'' in an extensive region below the neutrinosphere where the lepton number, $Y_{\ell}$, is small. | result 0.93 | 0.93 | 0.58 | asserted 1.00 |
| This instability is driven by a mechanism very different from that giving rise to neutron fingers, and may play an important role in enhancing the neutrino emission. | interpretation 0.97 | 0.66 | 0.24 | hedged possibility 0.90 |
| Deep in the core where the entropy is low and the lepton number higher, our analysis indicates a region unstable to another instability which we refer to as ``lepto-entropy semiconvection.'' These instabilities, particularly lepto-entropy fingers, may have already been seen in some multi-dimensional core collapse simulations described in the literature. | result 0.58 | 0.83 | 0.12 | hedged possibility 0.98 |
What kind of paper the classifier reports this is: theoretical result 0.53 · evidence from simulation or computation 0.89
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Compiled by classifier-1.13.0 via TypeSafe API, question bank abstract-p1-20260923, 2026-09-23: 1 request, 5,848 input tokens.
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7 arXiv papers cite this in 10 sentences
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However, this was later found to be incorrect [ref] , although PNS convection is still important in several aspects of CCSNe [ref] .
The physics of Core-Collapse Supernovae: explosion mechanism and explosive nucleosynthesis · Neutrino delayed heating · contest 0.78
Uses its method or tool 1 paper
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The BV frequency plotted here is given by [ref]
Gravitational-wave signal of a core-collapse supernova explosion of a 15 Solar mass star · Temporal Analysis · 0.95
Cites it as background 2 papers
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An interesting discussion on the relevance of this astrophysical fluid dynamics phenomenon and its timescale (1-50 ms) for the production of bursts of gravitational waves during the deleptonization phase of supernovae is given in Ref. [ref] . ] [ref] and the final explosion wind.
Probing nonlinear electrodynamics in slowly rotating spacetimes through neutrino astrophysics · Introduction · 0.80
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Further mixing processes near the proto-neutron star surface that could enhance the neutrino heating behind the shock include doubly diffusive instabilities [ref] , neutrino-bubble instabilities [ref] , and magnetic buoyancy instabilities [ref] .
Freeze-out yields of radioactivities in core-collapse supernovae · INTRODUCTION · 0.88
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