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Relativistic X-Ray Reverberation from Super-Eddington Accretion Flow

  • Authors: Lars Lund Thomsen, Lixin Dai, Erin Kara, and Chris Reynolds

2022 The Astrophysical Journal 925 151.

  • Provider: AAS Journals

Caption: Figure 4.

2D transfer functions for different super-Eddington (SE) and thin disk configurations. The BH spin a = 0.8 for all configurations. The x-axis shows the time delay of the reflected photons in gravitational units, which can be converted to real units as Rg/c ≈ 4.9 s × M6, with M6MBH/106 M. The energy shift is shown on the y-axis. Darker red color indicates stronger intensity Iobs. The 1D response function, Ψ(t), and the Fe Kα line profile, Ψ(E), are shown, respectively, in the bottom and left panels of each subfigure. For SE disks, we fix the inclination angle to i = 5°, and vary the optical depth of the reflection surface τ and the lamppost height hLP between 5 and 20 Rg in (a)–(d). As a comparison, for the thin disks, we have two inclination angles: face-on (i = 5°) (e) and edge-on (i = 80°) (f).

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