Journal ArticleDOI
Theory of pulsar magnetospheres
TLDR
In this article, a wide range of fundamental physical problems directly related to how pulsars function are discussed, some of which are independent of the specific pulsar mechanism and others relate directly to the physics of the pulsar and already shed some light on the properties of matter at high density and in strong magnetic fields.Abstract:
There is a wide range of fundamental physical problems directly related to how pulsars function. Some of these are independent of the specific pulsar mechanism. Others relate directly to the physics of the pulsar and already shed some light on the properties of matter at high density (\ensuremath{\sim}${10}^{15}$ g/cc) and in strong magnetic fields (\ensuremath{\sim}${10}^{12}$ G). Pulsars are assumed to be rotating neutron stars surrounded by strong magnetic fields and energetic particles. It is somewhere within this "magnetosphere" that the pulsar action is expected to take place. Currently there has been considerable difficulty in formulating an entirely self-consistent theory of the magnetospheric behavior and there may be rapid revisions in the near future, which is all the more surprising since many of the issues involve "elementary" problems in electromagnetism. One interesting discovery is that charge-separated plasmas apparently can support stable static discontinuities.read more
Citations
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Millisecond pulsars with extremely strong magnetic fields as a cosmological source of γ-ray bursts
TL;DR: In this article, a new model for γ-ray bursts at cosmological distances was proposed, based on the formation of rapidly rotating neutron stars with surface magnetic fields of the order of 1015.
Journal ArticleDOI
Nonlinear collective effects in photon-photon and photon-plasma interactions
TL;DR: In this paper, the authors considered strong field effects in laboratory and astrophysical plasmas and high intensity laser and cavity systems related to quantum electrodynamical (QED) photon-photon scattering.
Journal ArticleDOI
The Axisymmetric Pulsar Magnetosphere
TL;DR: In this article, the structure of the axisymmetric force-free magnetosphere of an aligned rotating magnetic dipole has been studied for the case that there exists a sufficiently large charge density to satisfy the ideal MHD condition, E B = 0, everywhere.
Journal ArticleDOI
Ion-acoustic solitons in electron-positron-ion plasmas
TL;DR: In this article, the ion-acoustic solitons were investigated in three-component plasmas, whose constituents are electrons, positrons, and singly charged ions.
Journal ArticleDOI
Reconnection in a striped pulsar wind
Yuri Lyubarsky,John G. Kirk +1 more
TL;DR: In this paper, it was shown that the wind accelerates significantly in the course of reconnection, which dilates the timescale over which the reconnection process operates, and requires a much larger distance than was previously thought to convert the Poynting flux to particle flux.
References
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Journal ArticleDOI
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J. R. Oppenheimer,G. M. Volkoff +1 more
TL;DR: In this paper, the authors studied the gravitational equilibrium of masses of neutrons, using the equation of state for a cold Fermi gas, and general relativity, and showed that for masses under 1/3, there are no static equilibrium solutions.
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Theory of pulsars: polar gaps, sparks, and coherent microwave radiation
Ruderman,P.G. Sutherland +1 more
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Observation of a Rapidly Pulsating Radio Source
TL;DR: In this article, the first report of a curious class of astronomical radio sources, distinguished by their rapid and extremely regular pulsations, was made by Hewish et al. They are now understood to be rapidly rotating, magnetized neutron stars, or pulsars.
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Discovery of a pulsar in a binary system
R. A. Hulse,J. H. Taylor +1 more
TL;DR: In this paper, a pulsar with a pulsation period that varies systematically between 0.058967 and 0.59045 sec over a cycle of 0.3230 d was detected.
Journal ArticleDOI
The Angular Momentum of the Solar Wind
Edmund J. Weber,Leverett Davis +1 more
TL;DR: Steady state model of solar wind flow in equatorial plane solved for radial and azimuthal motions, taking into account pressure gradient, magnetic field and gravitational effects as discussed by the authors.