Particle simulation for an axisymmetric pulsar magnetosphere

Tomohide Wada

doi:10.1017/S1743921312024799

Particle simulation for an axisymmetric pulsar magnetosphere

Tomohide Wada

Research output: Chapter in Book/Report/Conference proceeding › Conference contribution

Abstract

We developed a new particle simulation code which includes pair creation (magnetic pair creation and photon collision process), propagation of gamma-ray, inertia of particle, interaction of plasma and multi-pole stellar field for steady axisymmetric pulsar magnetosphere. The photon path is solved stochastically by an analytical solution of the mean free path of pair creation processes at the photon position. The superimposed quadrupole magnetic field forms asymmetric electrostatic clouds on tje poloidal plane and the accelerating region is different from the dipole case. Here, we demonstrate some results of a test run for our simulation. We will adopt the code for more complicated cases, such that all above-mentioned effects will be considered together in future work.

Original language	English
Title of host publication	Neutron Stars and Pulsars
Subtitle of host publication	Challenges and Opportunities after 80 years
Editors	Joeri Van Leeuwen
Pages	537-539
Number of pages	3
Edition	S291
DOIs	https://doi.org/10.1017/S1743921312024799
Publication status	Published - 2012 Aug 1

Publication series

Name	Proceedings of the International Astronomical Union
Number	S291
Volume	8
ISSN (Print)	1743-9213
ISSN (Electronic)	1743-9221

Keywords

plasmas
pulsars: general

ASJC Scopus subject areas

Medicine (miscellaneous)
Astronomy and Astrophysics
Nutrition and Dietetics
Public Health, Environmental and Occupational Health
Space and Planetary Science

UN SDGs

This output contributes to the following UN Sustainable Development Goals (SDGs)

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10.1017/S1743921312024799

Cite this

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title = "Particle simulation for an axisymmetric pulsar magnetosphere",

abstract = "We developed a new particle simulation code which includes pair creation (magnetic pair creation and photon collision process), propagation of gamma-ray, inertia of particle, interaction of plasma and multi-pole stellar field for steady axisymmetric pulsar magnetosphere. The photon path is solved stochastically by an analytical solution of the mean free path of pair creation processes at the photon position. The superimposed quadrupole magnetic field forms asymmetric electrostatic clouds on tje poloidal plane and the accelerating region is different from the dipole case. Here, we demonstrate some results of a test run for our simulation. We will adopt the code for more complicated cases, such that all above-mentioned effects will be considered together in future work.",

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PY - 2012/8/1

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N2 - We developed a new particle simulation code which includes pair creation (magnetic pair creation and photon collision process), propagation of gamma-ray, inertia of particle, interaction of plasma and multi-pole stellar field for steady axisymmetric pulsar magnetosphere. The photon path is solved stochastically by an analytical solution of the mean free path of pair creation processes at the photon position. The superimposed quadrupole magnetic field forms asymmetric electrostatic clouds on tje poloidal plane and the accelerating region is different from the dipole case. Here, we demonstrate some results of a test run for our simulation. We will adopt the code for more complicated cases, such that all above-mentioned effects will be considered together in future work.

AB - We developed a new particle simulation code which includes pair creation (magnetic pair creation and photon collision process), propagation of gamma-ray, inertia of particle, interaction of plasma and multi-pole stellar field for steady axisymmetric pulsar magnetosphere. The photon path is solved stochastically by an analytical solution of the mean free path of pair creation processes at the photon position. The superimposed quadrupole magnetic field forms asymmetric electrostatic clouds on tje poloidal plane and the accelerating region is different from the dipole case. Here, we demonstrate some results of a test run for our simulation. We will adopt the code for more complicated cases, such that all above-mentioned effects will be considered together in future work.

KW - plasmas

KW - pulsars: general

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DO - 10.1017/S1743921312024799

M3 - Conference contribution

AN - SCOPUS:84876577799

SN - 9781107033801

T3 - Proceedings of the International Astronomical Union

SP - 537

EP - 539

BT - Neutron Stars and Pulsars

A2 - Van Leeuwen, Joeri

ER -

Particle simulation for an axisymmetric pulsar magnetosphere

Abstract

Publication series

Keywords

ASJC Scopus subject areas

UN SDGs

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