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• W3123453640 abstract "Pulsars and central engines of long gamma-ray bursts – collapsars – may produce highly magnetized (Poynting-flux-dominated) outflows expanding in dense surroundings (interstellar medium or stellar material). For certain injection conditions, the magnetic flux of the wind cannot be accommodated within the cavity. In this case, ideal (non-dissipative) magnetohydrodynamics models, similar to the Kennel & Coroniti model of the Crab nebula, break down (the so-called ‘sigma problem’). This is typically taken to imply that the wind should become particle-dominated on scales much smaller than the size of the cavity. The wind is then slowed down by a fluid-type (low magnetization) reverse shock. Recent Fermi results, indicating that the synchrotron spectrum of the Crab nebula extends well beyond the upper limit of the most efficient radiation-reaction-limited acceleration, contradict the presence of a low-sigma reverse shock." @default.
• W3123453640 created "2021-02-01" @default.
• W3123453640 creator A5014609093 @default.
• W3123453640 date "2010-04-01" @default.
• W3123453640 modified "2023-09-26" @default.
• W3123453640 title "A high-sigma model of pulsar wind nebulae" @default.
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• W3123453640 doi "https://doi.org/10.1111/j.1365-2966.2010.16553.x" @default.
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