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Nonaxisymmetric Hall instability: A key to understanding magnetars
High Energy Astrophysical Phenomena · Submitted 10 Jan 2020
abstract compiled · 2026-09-23 · no language-model review
The authors' main claim This supports the viability of the mechanism, which has been proposed to explain magnetar outbursts.
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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.
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The abstract, sentence by sentence
It is generally accepted that the non-linear, dynamical evolution of magnetic fields in the interior of neutron stars plays a key role in the explanation of the observed phenomenology. Understanding the transfer of energy between toroidal and poloidal components, or between different scales, is of particular relevance. In this letter, we present the first 3D simulations of the Hall instability in a neutron star crust, confirming its existence for typical magnetar conditions. We confront our results to estimates obtained by a linear perturbation analysis, which discards any interpretation as numerical instabilities and confirms its physical origin. Interestingly, the Hall instability creates locally strong magnetic structures that occasionally can make the crust yield to the magnetic stresses and generates coronal loops, similarly as solar coronal loops find their way out through the photosphere. This supports the viability of the mechanism, which has been proposed to explain magnetar outbursts.
background contribution method result interpretation main claim
| # | sentence | role | the authors' own work | states the main conclusion | strength |
|---|---|---|---|---|---|
| s0 | It is generally accepted that the non-linear, dynamical evolution of magnetic fields in the interior of neutron stars plays a key role in the explanation of the observed phenomenology. | background 1.00 | 0.04 | 0.04 | asserted 0.90 |
| s1 | Understanding the transfer of energy between toroidal and poloidal components, or between different scales, is of particular relevance. | background 0.99 | 0.04 | 0.03 | asserted 0.94 |
| s2 | In this letter, we present the first 3D simulations of the Hall instability in a neutron star crust, confirming its existence for typical magnetar conditions. | contribution 0.99 | 0.97 | 0.34 | asserted 1.00 |
| s3 | We confront our results to estimates obtained by a linear perturbation analysis, which discards any interpretation as numerical instabilities and confirms its physical origin. | method 0.70 | 0.89 | 0.12 | asserted 1.00 |
| s4 | Interestingly, the Hall instability creates locally strong magnetic structures that occasionally can make the crust yield to the magnetic stresses and generates coronal loops, similarly as solar coronal loops find their way out through the photosphere. | result 0.67 | 0.85 | 0.26 | asserted 0.53 |
| s5 | This supports the viability of the mechanism, which has been proposed to explain magnetar outbursts. | interpretation 1.00 | 0.20 | 0.46 | hedged possibility 0.84 |
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The paper
Original abstract
It is generally accepted that the non-linear, dynamical evolution of magnetic fields in the interior of neutron stars plays a key role in the explanation of the observed phenomenology. Understanding the transfer of energy between toroidal and poloidal components, or between different scales, is of particular relevance. In this letter, we present the first 3D simulations of the Hall instability in a neutron star crust, confirming its existence for typical magnetar conditions. We confront our results to estimates obtained by a linear perturbation analysis, which discards any interpretation as numerical instabilities and confirms its physical origin. Interestingly, the Hall instability creates locally strong magnetic structures that occasionally can make the crust yield to the magnetic stresses and generates coronal loops, similarly as solar coronal loops find their way out through the photosphere. This supports the viability of the mechanism, which has been proposed to explain magnetar outbursts.
Human review
How the literature uses it
7 arXiv papers cite this in 8 sentences
Papers citing it · 6 sentences without a confident label
Cites it as background 2 papers
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Up until now most of the work has been focused on the NS crust when modeling B-evolution (e.g., [ref] ).
Magnetic field evolution timescales in superconducting neutron stars · Introduction · 0.96
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Magnetic field evolution in a magnetar crust involves an interplay among the Hall effect, Ohmic dissipation and plastic flow [ref] , involving instabilities on timescales $∼10^3 y$ [ref] and possibly evolution toward an attractor solution on timescales $∼10^5 y$ [ref] ,2014PhRvL.112q1101G.
Non-Axisymmetric Precession of Magnetars and Fast Radio Bursts · Magnetic Precession · 0.94
What it cites · 21 sentences without a confident label
Uses the method or tool of 2 papers
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([ref]) inside a spherical shell, using a version of the PARODY 3-D MHD code [ref] suitably adapted to NSs [ref] .
Three-dimensional simulations of the magnetic stress in a neutron star crust · Introduction · 1.00
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([ref]) inside a spherical shell, using a version of the PARODY 3-D MHD code [ref] suitably adapted to NSs [ref] .
Magnetic field evolution in magnetar crusts through three dimensional simulations · Introduction · 1.00
Compares with 3 papers
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Although similar structures had been observed before in previous simulations [ref] , their actual origin and the true nature of a possible instability had not been settled.
Three-dimensional simulations of the magnetic stress in a neutron star crust · Introduction · 0.82
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Although similar structures had been observed before in previous simulations [ref] , their actual origin and the true nature of a possible instability had not been settled.
Magnetic field evolution in magnetar crusts through three dimensional simulations · Introduction · 0.82
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Although similar structures had been observed before in previous simulations [ref] , their actual origin and the true nature of a possible instability had not been settled.
Magnetic Axis Drift and Magnetic Spot Formation in Neutron Stars with Toroidal Fields · Introduction · 0.82
Cites as background 8 papers
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We must note the distinction between the resistive Hall instability, which is essentially a tearing mode [ref] , and ideal instabilities which operate under infinite conductivity, for example, the density-shear instability requiring a density gradient [ref] , or the fast collisionless reconnection observed in the whistler frequency range [ref] .
Magnetar Activity via the Density-Shear Instability in Hall-MHD · Introduction · 0.96
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We must note the distinction between the resistive Hall instability, which is essentially a tearing mode [ref] , and ideal instabilities which operate under infinite conductivity, for example, the density-shear instability requiring a density gradient [ref] , or the fast collisionless reconnection observed in the whistler frequency range [ref] .
Resistive Tearing Instability in Electron-MHD: Application to Neutron Star Crusts · Introduction · 0.96
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We must note the distinction between the resistive Hall instability, which is essentially a tearing mode [ref] , and ideal instabilities which operate under infinite conductivity, for example, the density-shear instability requiring a density gradient [ref] , or the fast collisionless reconnection observed in the whistler frequency range [ref] .
Density-shear instability in electron MHD · Introduction · 0.96
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