Method of the Particle-in-Cell Simulation for the Y-Point in the Pulsar Magnetosphere

Umizaki, Mitsuhiro; Shibata, Shinpei

doi:10.1093/pasj/62.1.131

Cited by 10 publications

(8 citation statements)

References 10 publications

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“…Yuki & Shibata (2012) described very similar studies. Umizaki & Shibata (2010) focused on a detailed study of the Y-point in the aligned rotator, i.e. the cusp point of the last field line just grazing the light cylinder.…”

Section: Numerical Simulationsmentioning

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: Numerical Simulationsmentioning

confidence: 99%

Theory of pulsar magnetosphere and wind

Pétri

2016

J. Plasma Phys.

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“…The inner edge of the neutral sheet, which is the open-close boundary of the magnetic field structure, is called Y-point. Umizaki & Shibata (2010) studied the Y-point via an axisymmetric particle-in-cell simulation. They demonstrated that the magnetic reconnection occurred quasi-periodically and thereby plasma was heated and accelerated.…”

Section: Discussionmentioning

confidence: 99%

A Particle Simulation for the Pulsar Magnetosphere: Relationship of Polar Cap, Slot Gap, and Outer Gap

Yuki,

Shibata

2012

Preprint

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To explain the pulsed emission of the rotation powered pulsars from radio to gamma-ray, the polar cap models, the slot gap models, and the outer gap models are proposed. The recent observations suggest that these models are likely to co-exist in the same magnetosphere. If so, their mutual relation is known to be troublesome (Harding 2009) due to the boundary conditions and the direction of the current which are properly assumed in each acceleration models.We performed a particle simulation for the global magnetospheric structure. Based on the simulation, we present a new picture of the global structure of the pulsar magnetosphere. It is found that a new dead zone is formed along the current neutral line which separates the oppositely directed current. We shall call this the current-neutral zone. We suggest that the polar cap accelerators and the slot gaps locate above the current-neutral zone, and the outer gap exist between the current neutral zone and the traditional dead zone. We also give an estimate of the super-rotation region.

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“…We assume homogeneous wave fields in the direction perpendicular to the dipole geomagnetic field. The calculation is performed using the Buneman‐Boris method (Buneman, ; Umizaki & Shibata, ), which is suitable to follow trajectories of gyrating particles. Figure shows two examples of such calculations, as performed when the electrons are within the spatial and temporal domain of the wave profile.…”

Section: Theoretical Calculationsmentioning

confidence: 99%

Relativistic Electron Increase During Chorus Wave Activities on the 6–8 March 2016 Geomagnetic Storm

et al. 2017

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There was a geomagnetic storm on 6–8 March 2016, in which Van Allen Probes A and B separated by ∼2.5 h measured increase of relativistic electrons with energies approximately several hundred keV to 1 MeV. Simultaneously, chorus waves were measured by both Van Allen Probes and Magnetospheric Multiscale (MMS) mission. Some of the chorus elements were rising tones, possibly due to nonlinear effects. These measurements are compared with a nonlinear theory of chorus waves incorporating the inhomogeneity ratio and the field equation. From this theory, a chorus wave profile in time and one‐dimensional space is simulated. Test particle calculations are then performed in order to examine the energization rate of electrons. Some electrons are accelerated, although more electrons are decelerated. The measured time scale of the electron increase is inferred to be consistent with this nonlinear theory.

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Method of the Particle-in-Cell Simulation for the Y-Point in the Pulsar Magnetosphere

Cited by 10 publications

References 10 publications

Theory of pulsar magnetosphere and wind

Theory of pulsar magnetosphere and wind

A Particle Simulation for the Pulsar Magnetosphere: Relationship of Polar Cap, Slot Gap, and Outer Gap

Relativistic Electron Increase During Chorus Wave Activities on the 6–8 March 2016 Geomagnetic Storm

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