Trajectories and Radiation of Charged Particles in the Pulsar Magnetosphere

Abstract

Trajectories and radiation of the accelerating electrons are studied in the pulsar magnetosphere approximated as the electromagnetic field of the Deutsch's solutions. Because the electrons are accelerated rapidly to ultra-relativistic velocity near the neutron star surface, the electron velocity vector (and then its trajectory) is derived from the balance between Lorentz force and radiation reaction force, which makes the pitch angle between electron trajectories and magnetic field lines nonzero in most part of the magnetosphere. In such a case, the spectral energy distributions (SEDs) of synchro-curvature radiation for the accelerating electrons with a mono-energetic form are calculated. Our results indicate that: (i) the pitch angle is the function of electron position ($r,\theta ,\varphi$) in the open field line regions, and increases with increasing $r$ and $\theta$ as well as increasing the inclination angle; (ii) the radius of curvature becomes large along the particle trajectory, and (iii) the SED appears a double peak structure depending on the emission position, where the synchrotron radiation plays an important role in X-ray band and curvature radiation mainly works in GeV band, which is only determined by parameters $\alpha$ and $\zeta$

arXiv comment11 pages, 8 figures. Accepted by MNRAS

References in corpus (25)

• The Second Fermi Large Area Telescope Catalog of Gamma-ray Pulsars
• The First Fermi Large Area Telescope Catalog of Gamma-ray Pulsars
• 3FHL: The Third Catalog of Hard Fermi-LAT Sources
• Detection of 16 Gamma-Ray Pulsars Through Blind Frequency Searches Using the Fermi LAT
• Gamma Ray Pulsars: Emission from Extended Polar Cap Cascades
• Two-Pole Caustic Model for High-Energy Lightcurves of Pulsars
• High-Altitude Particle Acceleration and Radiation in Pulsar Slot Gaps
• Extended Acceleration in Slot Gaps and Pulsar High-Energy Emission
• Ab-initio pulsar magnetosphere: three-dimensional particle-in-cell simulations of oblique pulsars
• Modeling high-energy pulsar lightcurves from first principles
• Gamma-Ray Emission in Dissipative Pulsar Magnetospheres: From Theory to Fermi Observations
• 3D Kinetic Pulsar Magnetosphere Models: Connecting to Gamma-Ray Observations
• Polarization of high-energy pulsar radiation in the striped wind model
• The inner annular Gap for pulsar radiation: gamma-ray and radio emission
• Gamma-Ray Light Curves from Pulsar Magnetospheres with Finite Conductivity
• Radio-to-TeV Phase-resolved Emission from the Crab Pulsar: The Annular Gap Model
• Testing dissipative magnetosphere model light curves and spectra with FERMI pulsars
• Fermi Gamma-Ray Pulsars: Understanding the High-Energy Emission from Dissipative Magnetospheres
• Order parameters for the high-energy spectra of pulsars
• Synchro-curvature radiation of charged particles in the strong curved magnetic fields
• Gamma-ray Emission from the Vela Pulsar Modeled with the Annular Gap and Core Gap
• High-energy pulses and phase-resolved spectra by inverse Compton emission in the pulsar striped wind - Application to Geminga
• Hybrid Numerical Simulations of Pulsar Magnetospheres
• General-relativistic pulsar radio and high-energy emission
• Frequency resolved radio and high-energy emission of pulsars

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• Orbits of particles with magnetic dipole moment around magnetized Schwarzschild black holes: Applications to S2 star orbit
• A new radiation reaction approximation for particle dynamics in the strong field regime