RECORD
On the physics of cold MHD winds from oblique rotators
Astrophysics · Submitted 5 Jul 1999
abstract compiled · 2026-09-23 · no language-model review
The authors' main claim In particular, I argue that all radio pulsars are apparently the slow rotators ejecting the Poynting dominated relativistic wind.
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
I show that the self-consistent solution of the problem of MHD plasma flow in magnetosphere of an oblique rotator with an initially split-monopole magnetic field is reduced to the solution of the similar problem for the axisymmetric rotator. All properties of the MHD cold plasma flows from the axisymmetric rotators with the initially split-monopole magnetic field are valid for the oblique rotators as well. Rotational losses of the oblique rotator do not depend on the inclination angle and there is no temporal evolution of this angle. Self-consistent analytical and numerical solutions for the axisymmetric plasma flows obtained earlier show that the rotators can be divided on fast rotators ($\sigma_0/U_0^2 > 1$) and slow rotators ($\sigma_0/U_0^2 < 1$), where $\sigma_0$ is the ratio of the Poynting flux to the matter energy flux in the flow at the equator on the surface of the star, $U_0 = \gamma_0v_0/c$, $v_0$ and $\gamma_0$ are the initial velocity and Lorentz-factor of the plasma. The self-consistent approximate analytical solution for the plasma flow from the oblique rotator is obtained under the condition $\sigma_0/U_0^2 \ll 1$. Implications of these results for radio pulsars are discussed. In particular, I argue that all radio pulsars are apparently the slow rotators ejecting the Poynting dominated relativistic wind.
background contribution method result interpretation main claim
| # | sentence | role | the authors' own work | states the main conclusion | strength |
|---|---|---|---|---|---|
| s0 | I show that the self-consistent solution of the problem of MHD plasma flow in magnetosphere of an oblique rotator with an initially split-monopole magnetic field is reduced to the solution of the similar problem for the axisymmetric rotator. | result 0.65 | 0.92 | 0.49 | asserted 1.00 |
| s1 | All properties of the MHD cold plasma flows from the axisymmetric rotators with the initially split-monopole magnetic field are valid for the oblique rotators as well. | result 0.96 | 0.67 | 0.45 | asserted 1.00 |
| s2 | Rotational losses of the oblique rotator do not depend on the inclination angle and there is no temporal evolution of this angle. | result 1.00 | 0.83 | 0.26 | asserted 1.00 |
| s3 | Self-consistent analytical and numerical solutions for the axisymmetric plasma flows obtained earlier show that the rotators can be divided on fast rotators ($\sigma_0/U_0^2 > 1$) and slow rotators ($\sigma_0/U_0^2 < 1$), where $\sigma_0$ is the ratio of the Poynting flux to the matter energy flux in the flow at the equator on the surface of the star, $U_0 = \gamma_0v_0/c$, $v_0$ and $\gamma_0$ are the initial velocity and Lorentz-factor of the plasma. | background 0.95 | 0.24 | 0.08 | asserted 1.00 |
| s4 | The self-consistent approximate analytical solution for the plasma flow from the oblique rotator is obtained under the condition $\sigma_0/U_0^2 \ll 1$. | contribution 0.61 | 0.93 | 0.10 | asserted 1.00 |
| s5 | Implications of these results for radio pulsars are discussed. | interpretation 0.95 | 0.53 | 0.03 | unclear 0.75 |
| s6 | In particular, I argue that all radio pulsars are apparently the slow rotators ejecting the Poynting dominated relativistic wind. | interpretation 1.00 | 0.73 | 0.40 | hedged possibility 0.51 |
What was examined, and what was not
- arXiv listing abstract v1
- 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
I show that the self-consistent solution of the problem of MHD plasma flow in magnetosphere of an oblique rotator with an initially split-monopole magnetic field is reduced to the solution of the similar problem for the axisymmetric rotator. All properties of the MHD cold plasma flows from the axisymmetric rotators with the initially split-monopole magnetic field are valid for the oblique rotators as well. Rotational losses of the oblique rotator do not depend on the inclination angle and there is no temporal evolution of this angle. Self-consistent analytical and numerical solutions for the axisymmetric plasma flows obtained earlier show that the rotators can be divided on fast rotators ($\sigma_0/U_0^2 > 1$) and slow rotators ($\sigma_0/U_0^2 < 1$), where $\sigma_0$ is the ratio of the Poynting flux to the matter energy flux in the flow at the equator on the surface of the star, $U_0 = \gamma_0v_0/c$, $v_0$ and $\gamma_0$ are the initial velocity and Lorentz-factor of the plasma. The self-consistent approximate analytical solution for the plasma flow from the oblique rotator is obtained under the condition $\sigma_0/U_0^2 \ll 1$. Implications of these results for radio pulsars are discussed. In particular, I argue that all radio pulsars are apparently the slow rotators ejecting the Poynting dominated relativistic wind.
Human review
References
How the literature uses it
8 arXiv papers cite this in 14 sentences
Papers citing it · 13 sentences without a confident label
Cites it as background 1 paper
-
Theories of global magnetohydrodynamic (MHD) and particle-in-cell (PIC) simulations emphasise the light-cylinder region, at cylindrical radius $$, as the approximate site where the magnetosphere transitions into a toroidally dominated wind and an equatorial current sheet develops [ref] .
A common four-beam geometry reveals altitude-stratified GeV pulses in canonical young pulsars · Introduction · 0.88
Discussion
Know something about this paper? Leave a comment, or highlight any passage above to comment on it.