Acceleration of protons and electrons in the electromagnetic field of a rotating orthogonal magnetic dipole

Laue, H.; Thielheim, K. O.

doi:10.1086/191120

Cited by 16 publications

(12 citation statements)

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“…Finkbeiner, Herold & Ruder (1990) discussed the validity of the Lorentz-Dirac equation in pulsar magnetospheres. A detailed study by Laue & Thielheim (1986) integrating numerically the Lorentz-Dirac equation for electrons and protons showed the particle orbits and maximum attainable energy for a perpendicular rotator. The radiation reaction limit, much is simpler to implement as the full equation of motion, has been applied to solve the pulsar magnetosphere topology by Gruzinov (2012), Gruzinov (2013) and Contopoulos (2016a).…”

Section: Radiation Reaction Limitmentioning

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: Radiation Reaction Limitmentioning

confidence: 99%

Theory of pulsar magnetosphere and wind

Pétri

2016

J. Plasma Phys.

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“…Namely, consider the generalized function F (s) = δ(s 2 ) defined on the real half-line s ≥ 0 2 . Relations s 2 = 0, s > 0 are the one-dimensional analog of (8). We put by definition…”

Section: Regularizationmentioning

confidence: 99%

Radiation reaction and renormalization in classical electrodynamics of a point particle in any dimension

2002

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The effective equations of motion for a point charged particle taking account of radiation reaction are considered in various space-time dimensions. The divergencies steaming from the pointness of the particle are studied and the effective renormalization procedure is proposed encompassing uniformly the cases of all even dimensions. It is shown that in any dimension the classical electrodynamics is a renormalizable theory if not multiplicatively beyond d = 4. For the cases of three and six dimensions the covariant analogs of the Lorentz-Dirac equation are explicitly derived.

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“…Because of the very high Lorentz factors, radiation reaction cannot be ignored, as shown by Laue & Thielheim (1986). We plan to add this damped motion in an upcoming work.…”

Section: Resultsmentioning

confidence: 99%

Particle acceleration in neutron star ultra-strong electromagnetic fields

Tomczak

Pétri

2020

J. Plasma Phys.

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In this paper, we discuss the results of a new particle pusher in realistic ultra-strong electromagnetic fields such as those encountered around rotating neutron stars. After presenting the results of this algorithm in simple fields and comparing them to expected exact analytical solutions, we present new simulations for a rotating magnetic dipole in vacuum for a millisecond pulsar by using the Deutsch solution. Particles are injected within the magnetosphere, neglecting radiation reaction, interaction among them and their feedback on the fields. Our simulations are therefore not yet fully self-consistent because the Maxwell equations are not solved according to the current produced by these particles. The code highlights the symmetrical behaviour of particles of opposite charge to mass ratio, $q/m$ , with respect to the north and south hemispheres. The relativistic Lorentz factor $\gamma$ of the accelerated particles is proportional to this ratio $q/m$ : protons reach up to $\gamma _p \simeq 10^{10.7}$ , whereas electrons reach up to $\gamma _e \simeq 10^{14}$ . Our simulations show that particles could either be captured by the neutron star, trapped around it or ejected far from it, well outside the light cylinder. Actually, for a given charge to mass ratio, particles follow similar trajectories. These particle orbits show some depleted directions, especially at high magnetic inclination with respect to the rotation axis for positive charges and at low inclination for negative charges because of symmetry. Other directions are preferred and loaded with a high density of particles, some directions concentrating the highest or lowest acceleration efficiencies.

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Acceleration of protons and electrons in the electromagnetic field of a rotating orthogonal magnetic dipole

Cited by 16 publications

References 0 publications

Theory of pulsar magnetosphere and wind

Theory of pulsar magnetosphere and wind

Radiation reaction and renormalization in classical electrodynamics of a point particle in any dimension

Particle acceleration in neutron star ultra-strong electromagnetic fields

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