RECORD
General-relativistic electromagnetic fields around a slowly rotating neutron star: stationary vacuum solutions
General Relativity and Quantum Cosmology · Submitted 5 Aug 2013
abstract compiled · 2026-09-23 · no language-model review
The authors' main claim In this paper, we derive a general formalism to extend to general relativity the Deutsch field solution valid in vacuum space.
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
Pulsars are thought to be highly magnetized rotating neutron stars accelerating charged particles along magnetic field lines in their magnetosphere and visible as pulsed emission from the radio wavelength up to high energy X-rays and gamma-rays. Being highly compact objects with compactness close to $\Xi = R_s/R\approx0.5$, where $\Rs=2\,G\,M/c^2$ is the Schwarzschild radius and $\{M,R\}$ the mass and radius of the neutron star, general-relativistic effects become important close to their surface. This is especially true for the polar caps where radio emission is supposed to emanate from, leading to well defined signatures such as linear and circular polarization. In this paper, we derive a general formalism to extend to general relativity the Deutsch field solution valid in vacuum space. Thanks to a vector spherical harmonic expansion of the electromagnetic field, we are able to express the solution to any order in the spin parameter $\Omega$ of the compact object. We hope this analysis to serve as a benchmark to test numerical codes used to compute black hole and neutron star magnetospheres.
background contribution method result interpretation main claim
| # | sentence | role | the authors' own work | states the main conclusion | strength |
|---|---|---|---|---|---|
| s0 | Pulsars are thought to be highly magnetized rotating neutron stars accelerating charged particles along magnetic field lines in their magnetosphere and visible as pulsed emission from the radio wavelength up to high energy X-rays and gamma-rays. | background 1.00 | 0.04 | 0.03 | hedged possibility 0.89 |
| s1 | Being highly compact objects with compactness close to $\Xi = R_s/R\approx0.5$, where $\Rs=2\,G\,M/c^2$ is the Schwarzschild radius and $\{M,R\}$ the mass and radius of the neutron star, general-relativistic effects become important close to their surface. | background 1.00 | 0.06 | 0.02 | asserted 0.99 |
| s2 | This is especially true for the polar caps where radio emission is supposed to emanate from, leading to well defined signatures such as linear and circular polarization. | background 0.99 | 0.05 | 0.02 | asserted 0.59 |
| s3 | In this paper, we derive a general formalism to extend to general relativity the Deutsch field solution valid in vacuum space. | contribution 0.99 | 0.95 | 0.23 | asserted 0.99 |
| s4 | Thanks to a vector spherical harmonic expansion of the electromagnetic field, we are able to express the solution to any order in the spin parameter $\Omega$ of the compact object. | method 0.98 | 0.94 | 0.16 | asserted 1.00 |
| s5 | We hope this analysis to serve as a benchmark to test numerical codes used to compute black hole and neutron star magnetospheres. | future work 0.97 | 0.14 | 0.11 | hedged possibility 0.53 |
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
Pulsars are thought to be highly magnetized rotating neutron stars accelerating charged particles along magnetic field lines in their magnetosphere and visible as pulsed emission from the radio wavelength up to high energy X-rays and gamma-rays. Being highly compact objects with compactness close to $\Xi = R_s/R\approx0.5$, where $\Rs=2\,G\,M/c^2$ is the Schwarzschild radius and $\{M,R\}$ the mass and radius of the neutron star, general-relativistic effects become important close to their surface. This is especially true for the polar caps where radio emission is supposed to emanate from, leading to well defined signatures such as linear and circular polarization. In this paper, we derive a general formalism to extend to general relativity the Deutsch field solution valid in vacuum space. Thanks to a vector spherical harmonic expansion of the electromagnetic field, we are able to express the solution to any order in the spin parameter $\Omega$ of the compact object. We hope this analysis to serve as a benchmark to test numerical codes used to compute black hole and neutron star magnetospheres.
Human review
References
How the literature uses it
1 arXiv paper cite this in 2 sentences
Papers citing it
Cites it as background 1 paper
-
[ref] , [ref] , [ref] and [ref] computed the effects of general relativity on the electromagnetic field around a slowly rotating neutron star.
Theory of pulsar magnetosphere and wind · General relativity · 0.80
Discussion
Know something about this paper? Leave a comment, or highlight any passage above to comment on it.