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Axisymmetric pulsar magnetosphere revisited
High Energy Astrophysical Phenomena · Submitted 8 Sep 2021
abstract compiled · 2026-09-23 · no language-model review
The authors' main claim A much higher power is released in the equatorial plane, especially at the Y-point where the created dense $e^\pm$ plasma is spun up and intermittently ejected through the nozzle between the two open magnetic fluxes.
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The abstract, sentence by sentence
We present a global kinetic plasma simulation of an axisymmetric pulsar magnetosphere with self-consistent $e^\pm$ pair production. We use the particle-in-cell method and log-spherical coordinates with a grid size $4096\times 4096$. This allows us to achieve a high voltage induced by the pulsar rotation and investigate pair creation in a young pulsar far from the death line. We find the following. (1) The energy release and $e^\pm$ creation are strongly concentrated in the thin, Y-shaped current sheet, with a peak localized in a small volume at the Y-point. (2) The Y-point is shifted inward from the light cylinder by $\sim 15\%$, and "breathes" with a small amplitude. (3) The dense $e^\pm$ cloud at the Y-point is in ultra-relativistic rotation, which we call super-rotation, because it exceeds co-rotation with the star. The cloud receives angular momentum flowing from the star along the poloidal magnetic lines. (4) Gamma-ray emission peaks at the Y-point and is collimated in the azimuthal direction, tangent to the Y-point circle. (5) The separatrix current sheet between the closed magnetosphere and the open magnetic field lines is sustained by the electron backflow from the Y-point cloud. Its thickness is self-regulated to marginal charge starvation. (6) Only a small fraction of dissipation occurs in the separatrix inward of the Y-point. A much higher power is released in the equatorial plane, especially at the Y-point where the created dense $e^\pm$ plasma is spun up and intermittently ejected through the nozzle between the two open magnetic fluxes.
background contribution method result interpretation main claim
| # | sentence | role | the authors' own work | states the main conclusion | strength |
|---|---|---|---|---|---|
| s0 | We present a global kinetic plasma simulation of an axisymmetric pulsar magnetosphere with self-consistent $e^\pm$ pair production. | contribution 1.00 | 0.96 | 0.06 | asserted 0.98 |
| s1 | We use the particle-in-cell method and log-spherical coordinates with a grid size $4096\times 4096$. | method 1.00 | 0.93 | 0.02 | asserted 0.99 |
| s2 | This allows us to achieve a high voltage induced by the pulsar rotation and investigate pair creation in a young pulsar far from the death line. We find the following. | method 0.58 | 0.70 | 0.05 | asserted 0.95 |
| s3 | (1) The energy release and $e^\pm$ creation are strongly concentrated in the thin, Y-shaped current sheet, with a peak localized in a small volume at the Y-point. | result 1.00 | 0.96 | 0.29 | asserted 1.00 |
| s4 | (2) The Y-point is shifted inward from the light cylinder by $\sim 15\%$, and "breathes" with a small amplitude. | result 1.00 | 0.96 | 0.09 | asserted 1.00 |
| s5 | (3) The dense $e^\pm$ cloud at the Y-point is in ultra-relativistic rotation, which we call super-rotation, because it exceeds co-rotation with the star. | result 0.98 | 0.95 | 0.17 | asserted 1.00 |
| s6 | The cloud receives angular momentum flowing from the star along the poloidal magnetic lines. | interpretation 0.70 | 0.81 | 0.06 | asserted 1.00 |
| s7 | (4) Gamma-ray emission peaks at the Y-point and is collimated in the azimuthal direction, tangent to the Y-point circle. | result 1.00 | 0.94 | 0.13 | asserted 1.00 |
| s8 | (5) The separatrix current sheet between the closed magnetosphere and the open magnetic field lines is sustained by the electron backflow from the Y-point cloud. | result 1.00 | 0.91 | 0.10 | asserted 1.00 |
| s9 | Its thickness is self-regulated to marginal charge starvation. | result 0.98 | 0.87 | 0.06 | asserted 1.00 |
| s10 | (6) Only a small fraction of dissipation occurs in the separatrix inward of the Y-point. | result 1.00 | 0.93 | 0.07 | asserted 1.00 |
| s11 | A much higher power is released in the equatorial plane, especially at the Y-point where the created dense $e^\pm$ plasma is spun up and intermittently ejected through the nozzle between the two open magnetic fluxes. | result 0.96 | 0.94 | 0.35 | asserted 1.00 |
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The paper
Original abstract
We present a global kinetic plasma simulation of an axisymmetric pulsar magnetosphere with self-consistent $e^\pm$ pair production. We use the particle-in-cell method and log-spherical coordinates with a grid size $4096\times 4096$. This allows us to achieve a high voltage induced by the pulsar rotation and investigate pair creation in a young pulsar far from the death line. We find the following. (1) The energy release and $e^\pm$ creation are strongly concentrated in the thin, Y-shaped current sheet, with a peak localized in a small volume at the Y-point. (2) The Y-point is shifted inward from the light cylinder by $\sim 15\%$, and "breathes" with a small amplitude. (3) The dense $e^\pm$ cloud at the Y-point is in ultra-relativistic rotation, which we call super-rotation, because it exceeds co-rotation with the star. The cloud receives angular momentum flowing from the star along the poloidal magnetic lines. (4) Gamma-ray emission peaks at the Y-point and is collimated in the azimuthal direction, tangent to the Y-point circle. (5) The separatrix current sheet between the closed magnetosphere and the open magnetic field lines is sustained by the electron backflow from the Y-point cloud. Its thickness is self-regulated to marginal charge starvation. (6) Only a small fraction of dissipation occurs in the separatrix inward of the Y-point. A much higher power is released in the equatorial plane, especially at the Y-point where the created dense $e^\pm$ plasma is spun up and intermittently ejected through the nozzle between the two open magnetic fluxes.
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6 arXiv papers cite this in 6 sentences
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Compares with it 1 paper
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Some of the previous 2D axisymmetric simulations of aligned pulsars [ref] reported the presence of excess dissipation near the Y-point, at the level of a few percent of $L_0$, with a lower dissipation rate at $r>R_LC$.
Magnetic energy dissipation and gamma-ray emission in energetic pulsars · Magnetic energy dissipation via reconnection · 0.82
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