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Monster Radiative Shocks in the Perturbed Magnetospheres of Neutron Stars

  • Authors: Andrei M. Beloborodov

Andrei M. Beloborodov 2023 The Astrophysical Journal 959 .

  • Provider: AAS Journals

Caption: Figure 3.

Schematic illustration of the flow of characteristics C + in FFE and MHD, shown in the tξ plane. Each C + has its initial position ξ i and carries a value of ﹩K({\xi }_{{\rm{i}}})={rE}/\mu ﹩ determined by the initial wave profile. In the FFE limit, the characteristics are vertical straight lines; they propagate with speed β + = 1, which corresponds to d ξ +/dt = 0. The MHD correction to FFE implies d ξ +/dt = 1 − β + ≠ 0, so the C + characteristics are no longer static in ξ; they become significantly bent in the region where E 2 approaches B 2, leading to the formation of a shock (red curve).

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