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The Boomerang PWN G106.6+2.9 and the Magnetic Field Structure in Pulsar Wind Nebulae

  • Authors: Roland Kothes, Wolfgang Reich, and Bülent Uyanıker

Kothes, Reich, & Uyanıker 2006 The Astrophysical Journal 638 225.

  • Provider: AAS Journals

Caption: Fig. 8.

Magnetic field strength B as a function of the age of the Boomerang tPWN. The solid line was calculated from the total energy content of the nebula (eq.[ 4]) assuming equipartition. The dashed line represents the magnetic field necessary to create the spectral break at 4.3 GHz (eq. [1]). The point at which the curves intersect determines the age of the nebula and the magnetic field.

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