Pulsar striped winds
arXiv:1702.00720 · doi:10.1007/978-3-319-63031-1_7
Abstract
According to magnetohydrodynamic (MHD) models, the rotational energy of a rapidly spinning neutron star is carried away by a relativistic wind and deposited at a large distance, in the nebula, downstream of the wind termination shock. The energy transport in the outflow is mediated by Poynting flux, but it is not clear how the energy stored in the fields is transferred into the energized population of emitting particles. The most plausible dissipation mechanisms are thought to be related to the "striped" structure of the wind, in particular, to the existence of a current sheet, prone to reconnection events. In this model the current sheet is a natural place for internal dissipation and acceleration of particles responsible for pulsed, high-energy emission. Moreover, reconnection is a promising scenario for explaining annihilation of fields at the shock and conversion of their energy into the kinetic energy of particles. The shock structure, however, is likely to differ in the low-density plasmas, in which non-MHD effects intervene. In this regime, the striped wind can dissipate its energy via an electromagnetic precursor of the shock.
invited review at the Workshop on Modelling Nebulae, June 14-17, 2016, Sant Cugat, Spain; submitted book chapter
References in corpus (13)
- Formation of Hard Power-laws in the Energetic Particle Spectra Resulting from Relativistic Magnetic Reconnection
- Ab-initio pulsar magnetosphere: three-dimensional particle-in-cell simulations of oblique pulsars
- Discovery of High-Energy Gamma-Ray Emission from the Binary System PSR B1259-63/LS 2883 Around Periastron with Fermi
- Particle acceleration in axisymmetric pulsar current sheets
- Relativistic magnetic reconnection in pair plasmas and its astrophysical applications
- Multipolar electromagnetic fields around neutron stars: exact vacuum solutions and related properties
- Very high energy emission as a probe of relativistic magnetic reconnection in pulsar winds
- Fermi-LAT Detection of Pulsed Gamma-rays Above 50 GeV from the Vela Pulsar
- High-energy observations of PSR B1259-63/LS 2883 through the 2014 periastron passage: connecting X-rays to the GeV flare
- Modeling of the gamma-ray pulsed spectra of Geminga, Crab, and Vela with synchro-curvature radiation
- Axisymmetric force-free magnetosphere of a pulsar. II. Transition from the self-consistent two-fluid model
- Magnetic reconnection at the termination shock in a striped pulsar wind
- A novel look at the pulsar force-free magnetosphere