Spin and Accretion Rate Dependence of Black Hole X-Ray Spectra
We present a survey of how the spectral features of black hole X-ray binary systems depend on spin, accretion rate, viewing angle, and Fe abundance when predicted on the basis of first-principles physical calculations. The power-law component hardens with increasing spin. The thermal component stren...
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| Veröffentlicht in: | The Astrophysical journal 2021-12, Vol.922 (2), p.270 |
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| creator | Kinch, Brooks E. Schnittman, Jeremy D. Noble, Scott C. Kallman, Timothy R. Krolik, Julian H. |
| description | We present a survey of how the spectral features of black hole X-ray binary systems depend on spin, accretion rate, viewing angle, and Fe abundance when predicted on the basis of first-principles physical calculations. The power-law component hardens with increasing spin. The thermal component strengthens with increasing accretion rate. The Compton bump is enhanced by higher accretion rate and lower spin. The Fe Kα equivalent width grows sublinearly with Fe abundance. Strikingly, the Kα profile is more sensitive to accretion rate than to spin because its radial surface brightness profile is relatively flat, and higher accretion rate extends the production region to smaller radii. The overall radiative efficiency is at least 30%–100% greater than as predicted by the Novikov–Thorne model. |
| doi_str_mv | 10.3847/1538-4357/ac2b9a |
| format | Article |
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| subjects | Accretion Astronomy ASTRONOMY AND ASTROPHYSICS Astrophysics Black holes Deposition First principles General relativity Magnetohydrodynamical simulations Surface brightness X ray binaries X ray spectra X ray stars X-ray astronomy X-ray binary stars |
| title | Spin and Accretion Rate Dependence of Black Hole X-Ray Spectra |
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