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Resonant Inverse Compton Scattering Spectra from Highly Magnetized Neutron Stars

  • Authors: Zorawar Wadiasingh, Matthew G. Baring, Peter L. Gonthier, and Alice K. Harding

2018 The Astrophysical Journal 854 98.

  • Provider: AAS Journals

Caption: Figure 9.

Spectra IV: meridional field loops at ﹩{\gamma }_{e}={10}^{2}﹩ (left) and ﹩{\gamma }_{e}={10}^{1.5}﹩ (right) as a function of viewing angle, both with ﹩{r}_{\max }=4﹩ but differing in local ﹩{\boldsymbol{B}}﹩. Solid curves represent spectra computed with the full Sokolov & Ternov (ST) cross section in QED, i.e., Equation (25); dashed (﹩\perp ﹩ mode) and dot-dashed (﹩\parallel ﹩ mode) curves in the left panel define spectra determined using the magnetic Thomson cross section instead (see text). The left panel has relatively high local field at the resonant interaction point, since ﹩{B}_{p}=100﹩, while the right panel illustrates the same parameters as those in Figure 8 but with ﹩{\gamma }_{e}={10}^{1.5}﹩. It is apparent that polarization ﹩\perp ﹩ (solid curves) exceeds ﹩\parallel ﹩ (dotted curves) in the 0.05–1 MeV hard X-ray band for most viewing angles where head-on resonant interactions are sampled.

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