Time-dependent force-free pulsar magnetospheres: axisymmetric and oblique rotators
read the original abstract
Magnetospheres of many astrophysical objects can be accurately described by the low-inertia (or "force-free") limit of MHD. We present a new numerical method for solution of equations of force-free relativistic MHD based on the finite-difference time-domain (FDTD) approach with a prescription for handling spontaneous formation of current sheets. We use this method to study the time-dependent evolution of pulsar magnetospheres in both aligned and oblique magnetic geometries. For the aligned rotator we confirm the general properties of the time-independent solution of Contopoulos et al. (1999). For the oblique rotator we present the 3D structure of the magnetosphere and compute, for the first time, the spindown power of pulsars as a function of inclination of the magnetic axis. We find the pulsar spindown luminosity to be L = (mu^2 Omega^4/c^3) (1+ sin^2(alpha)) for a star with the dipole moment "mu", rotation frequency "Omega", and magnetic inclination angle "alpha". We also discuss the effects of current sheet resistivity and reconnection on the structure and evolution of the magnetosphere.
This paper has not been read by Pith yet.
Forward citations
Cited by 4 Pith papers
-
General-relativistic resistive-magnetohydrodynamics simulations of self-consistent magnetized rotating neutron stars
Resistive GRMHD simulations of rotating neutron stars show resistivity changes magnetic field geometries, suppresses instabilities, and lowers GW emission amplitude while maintaining a consistent 9:1 poloidal-to-toroi...
-
Crust glass formation reveals the neutron star birth properties in IGR J17480-2446
Accretion-induced failure of the neutron star crystal crust produces a glass layer that explains the observed cooling, fixes the accreted mass at 2.4e-6 solar masses, and indicates birth properties typical of recycled...
-
Old and Bright: The Remarkable Radio Brightening of the Engine-driven SN 2012au Several Years After Explosion Signals the Birth of a PWN
Late-time radio observations of SN 2012au show re-brightening best explained by emission from a newborn pulsar wind nebula rather than continued shock interaction with circumstellar material.
-
A Log-Uniform Initial Magnetic Field Distribution Explains Pulsar and Magnetar Populations through Magnetic Inclination Alignment
Magnetic inclination alignment with timescale proportional to B to the minus two suppresses observed numbers of strong-field neutron stars, unifying pulsars and magnetars under one log-uniform initial B distribution.
discussion (0)
Sign in with ORCID, Apple, or X to comment. Anyone can read and Pith papers without signing in.