The radiation of rotating magnetic dipoles in vacuo in general relativity

Pfarr, Joachim

doi:10.1007/bf00766140

Cited by 5 publications

(2 citation statements)

References 16 publications

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“…This demonstrated clearly that a quantitative analysis of the acceleration processes and radiation in the vicinity of the neutron star can only be done by a treatment of the Maxwell equations in the presence of a strong gravitational field. In this way Pfarr (1976) looked for an approximate solution to the Maxwell equations in curved space–time, Schwarzschild or Kerr, through a linearized approach using the Newman–Penrose formalism (Newman & Penrose 1962). He computed the emission of electromagnetic waves in vacuum for a rotating dipole in general relativity with an expression for the Poynting flux depending on .…”

Section: Other Effects On the Magnetospherementioning

confidence: 99%

Theory of pulsar magnetosphere and wind

Pétri

2016

J. Plasma Phys.

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Neutron stars are fascinating astrophysical objects immersed in strong gravitational and electromagnetic fields, at the edge of our current theories. These stars manifest themselves mostly as pulsars, emitting a timely very stable and regular electromagnetic signal. Even though discovered almost fifty years ago, they still remain mysterious compact stellar objects. In this review, we summarize the most fundamental theoretical aspects of neutron star magnetospheres and winds. The main competing models explaining their radiative properties like multi-wavelength pulse shapes and spectra and the underlying physical processes such as pair creation and radiation mechanisms are scrutinized. A global but still rather qualitative picture slowly emerges thanks to recent advances in numerical simulations on the largest scales. However considerations about pulsar magnetospheres remain speculative. For instance, the exact composition of the magnetospheric plasma is not yet known. Is it solely filled with a mixture of e ± leptons or does it contain a non-negligible fraction of protons and/or ions? Is it almost entirely filled or mostly empty except for some small anecdotal plasma filled regions? Answers to these questions will strongly direct the description of the magnetosphere to seemingly contradictory results leading sometimes to inconsistencies. Nevertheless, accounts are given as to the latest developments in the theory of pulsar magnetospheres and winds, the existence of a possible electrosphere and physical insight obtained from related observational signatures of multi-wavelength pulsed emission.

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Section: Other Effects On the Magnetospherementioning

confidence: 99%

Theory of pulsar magnetosphere and wind

Pétri

2016

J. Plasma Phys.

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“…It is therefore crucial to treat Maxwell equations in the general-relativistic framework in order to analyse quantitatively acceleration and radiation in the vicinity of the neutron star. This led Pfarr (1976) to seek for an approximate solution of…”

Section: Introductionmentioning

confidence: 99%

General-relativistic electromagnetic fields around a slowly rotating neutron star: stationary vacuum solutions

Pétri

2013

Monthly Notices of the Royal Astronomical Society

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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 Xrays and gamma-rays. Being highly compact objects with compactness close to Ξ = R s /R ≈ 0.5, where R s = 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 Ω 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.

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Neutron star electrodynamics in curved space

Cohen

Kearney

1980

Astrophys Space Sci

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The radiation of rotating magnetic dipoles in vacuo in general relativity

Cited by 5 publications

References 16 publications

Theory of pulsar magnetosphere and wind

Theory of pulsar magnetosphere and wind

General-relativistic electromagnetic fields around a slowly rotating neutron star: stationary vacuum solutions

Neutron star electrodynamics in curved space

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