2016/12/07 by Jonathan Zrake, Jonathan Arons · 39 citations
Physics and Astronomy · #Astrophysics #Computational physics #Crab Nebula #Gamma-ray burst #Gamma-ray bursts and supernovae #Magnetar #Magnetic energy #Magnetic field #Magnetohydrodynamics #Millisecond pulsar #Nebula #Neutron star #Physics #Pulsar #Pulsars and Gravitational Waves Research #Solar and Space Plasma Dynamics #astro-ph.HE
paper · pdf · doi:10.3847/1538-4357/aa826d
published in The Astrophysical Journal 847(1), 57 (IOP Publishing) · Submitted to ApJ
arxiv created 2016/12/07 · openalex publication_date 2017/09/20 · arxiv updated 2017/09/27 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05
Abstract We present a model for magnetic energy dissipation in a pulsar wind nebula. A better understanding of this process is required to assess the likelihood that certain astrophysical transients may be powered by the spin-down of a “millisecond magnetar.” Examples include superluminous supernovae, gamma-ray bursts, and anticipated electromagnetic counterparts to gravitational wave detections of binary neutron star coalescence. Our model leverages recent progress in the theory of turbulent magnetic relaxation to specify a dissipative closure of the stationary magnetohydrodynamic (MHD) wind equations, yielding predictions of the magnetic energy dissipation rate throughout the nebula. Synchrotron losses are self-consistently treated. To demonstrate the model’s efficacy, we show that it can reproduce many features of the Crab Nebula, including its expansion speed, radiative efficiency, peak photon energy, and mean magnetic field strength. Unlike ideal MHD models of the Crab (which lead to the so-called σ -problem), our model accounts for the transition from ultra to weakly magnetized plasma flow and for the associated heating of relativistic electrons. We discuss how the predicted heating rates may be utilized to improve upon models of particle transport and acceleration in pulsar wind nebulae. We also discuss implications for the Crab Nebula’s γ -ray flares, and point out potential modifications to models of astrophysical transients invoking the spin-down of a millisecond magnetar.