2002/02/19 by Maxim Lyutikov · 33 citations
Physics and Astronomy · #Astrophysics #Astrophysics and Cosmic Phenomena #Classical mechanics #Context (archaeology) #Gamma-ray bursts and supernovae #Kinetic energy #Magnetic field #Magnetohydrodynamics #Mass flux #Mechanics #Nuclear physics #Physics #Plasma #Pulsar #Pulsars and Gravitational Waves Research #Radiative transfer #Shock (circulatory) #Shock wave #Toroid #astro-ph
paper · pdf · doi:10.1046/j.1365-8711.2003.06141.x
published in Monthly Notices of the Royal Astronomical Society 339(3), 623-632 (Oxford University Press) · 24 pages, 4 figures
arxiv created 2002/02/19 · openalex publication_date 2003/03/01 · arxiv updated 2009/12/01 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05
The dynamics of relativistic magnetized mass-loaded outflows carrying the toroidal magnetic field is analysed in the context of pulsar wind nebulae (PWNs). Mass-loading is very efficient in slowing down super-relativistic magnetized flows and weakening relativistic shocks. We suggest that the weakening of relativistic reverse shocks by mass-loading in PWNs is responsible for the low radiative efficiencies of the majority of the PWNs. Mass-loading may also result in a shock transition near the fast magnetosonic point; this is unlikely to happen in the majority of PWNs. The evolution of magnetized mass-loaded flows beyond the reverse shock is complicated: after the initial deceleration to the minimal velocity required to transport the magnetic flux, the mass-loaded flows have to accelerate. This formally precludes mass-loaded flows carrying ordered toroidal magnetic field from reaching infinity. The final outcome of mass loading of magnetized winds remains uncertain and may depend on kinetic details of how mass loading occurs.