34 research outputs found
Three-dimensional numerical simulations of the pulsar magentoshere: Preliminary results
We investigate the three-dimensional structure of the pulsar magnetosphere
through time-dependent numerical simulations of a magnetic dipole that is set
in rotation. We developed our own Eulerian finite difference time domain
numerical solver of force-free electrodynamics and implemented the technique of
non-reflecting and absorbing outer boundaries. This allows us to run our
simulations for many stellar rotations, and thus claim with confidence that we
have reached a steady state. A quasi-stationary corotating pattern is
established, in agreement with previous numerical solutions. We discuss the
prospects of our code for future high-resolution investigations of dissipation,
particle acceleration, and temporal variability.Comment: 9 pages, 4 figures. Astronomy & Astrophysics, in pres
MeV Pulsars: Modeling Spectra and Polarization
A sub-population of energetic rotation-powered pulsars show high fluxes of
pulsed non-thermal hard X-ray emission. While this MeV pulsar population
includes some radio-loud pulsars like the Crab, a significant number have no
detected radio or GeV emission, a mystery since gamma- ray emission is a common
characteristic of pulsars with high spin-down power. Their steeply rising hard
X-ray spectral energy distributions (SEDs) suggest peaks at 0.1 - 1 MeV but
they have not been detected above 200 keV. Several upcoming and planned
telescopes may shed light on the MeV pulsars. The Neutron star Interior
Composition ExploreR (NICER) will observe pulsars in the 0.2 - 12 keV band and
may discover additional MeV pulsars. Planned telescopes, such as All-Sky
Medium-Energy Gamma-Ray Observatory (AMEGO) and e-ASTROGAM, will detect
emission above 0.2 MeV and polarization in the 0.2 - 10 MeV band. We present a
model for the spectrum and polarization of MeV pulsars where the X-ray emission
comes from electron- positron pairs radiating in the outer magnetosphere and
current sheet. This model predicts that the peak of the SED increases with
surface magnetic field strength if the pairs are produced in polar cap
cascades. For small inclination angles, a range of viewing angles can miss both
the radio pulse and the GeV pulse from particles accelerating near the current
sheet. Characterizing the emission and geometry of MeV pulsars can thus provide
clues to the source of pairs and acceleration in the magnetosphere.Comment: 8 pages, 5 figures, published in Proceedings of Scienc
The Extended Pulsar Magnetosphere
We present the structure of the 3D ideal MHD pulsar magnetosphere to a radius ten times that of the light cylinder, a distance about an order of magnitude larger than any previous such numerical treatment. Its overall structure exhibits a stable, smooth, well-defined undulating current sheet which approaches the kinematic split monopole solution of Bogovalov 1999 only after a careful introduction of diffusivity even in the highest resolution simulations. It also exhibits an intriguing spiral region at the crossing of two zero charge surfaces on the current sheet, which shows a destabilizing behavior more prominent in higher resolution simulations. We discuss the possibility that this region is physically (and not numerically) unstable. Finally, we present the spiral pulsar antenna radiation pattern