Model of dynamical structures in synchrotron images of pulsar wind nebulae

17th Russian Youth Conference on Physics and Astronomy

物理学;天文学

Petrov, A.E.^1,2 ; Bykov, A.M.^1,2

Department of Cosmic Research, Saint-Petersburg State Polytechnical University, Polytekhnicheskaya st. 29, St. Petersburg

195251, Russia^1

Laboratory for High Energy Astrophysics, Ioffe Physical Technical Institute, Polytekhnicheskaya st. 26, St. Petersburg

194021, Russia^2

关键词: Dynamical structure;    Electromagnetic spectra;    Ground-based telescopes;    High angular resolutions;    Non-equilibrium process;    Non-thermal radiation;    Physical interpretation;    Stochastic magnetic field;   

Others  :  https://iopscience.iop.org/article/10.1088/1742-6596/661/1/012010/pdf
DOI  :  10.1088/1742-6596/661/1/012010

学科分类：天文学(综合)

来源: IOP

【 摘 要 】

The relativistic pulsar winds are forming the pulsar wind nebulae (PWN) - the unique extended sources of non-thermal radiation detected in all bands of the electromagnetic spectrum. High angular resolution imaging of the PWN with modern orbital and ground-based telescopes makes possible to study the highly non-equilibrium processes in the pulsar wind plasma. Physical interpretation of the observed dynamic structures in the nebulae requires modeling of the relativistic pulsar wind. The main mechanism of emission of the magnetized relativistic pair plasma in the PWN is the synchrotron radiation, and the observed dynamical structures may be related with a propagation of perturbations of the magnetic field. A kinetic approach to highly non-equilibrium relativistic pair plasma allows us to evaluate the structure of the perturbation of the magnetic field propagating transverse to the mean quasi-stationary magnetic field. We present synchrotron images with the dynamic structures in the PWN simulated in the relativistic pair plasma with the strong scattering of pairs by the stochastic magnetic field fluctuation.