SPH simulations of zero-energy partial TDEs find fallback ~t^{-9/4}, optical luminosities 10^{42-44} erg/s at 10^4 K and radii 10-100 au, indicating many detected TDEs may be partial rather than full.
A Grid of Relativistic, non-LTE Accretion Disk Models for Spectral Fitting of Black Hole Binaries
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abstract
Self-consistent vertical structure models together with non-LTE radiative transfer should produce spectra from accretion disks around black holes which differ from multitemperature blackbodies at levels which may be observed. High resolution, high signal-to-noise observations warrant spectral modeling which both accounts for relativistic effects, and treats the physics of radiative transfer in detail. In Davis et al. (2005) we presented spectral models which accounted for non-LTE effects, Compton scattering, and the opacities due to ions of abundant metals. Using a modification of this method, we have tabulated spectra for black hole masses typical of Galactic binaries. We make them publicly available for spectral fitting as an Xspec model. These models represent the most complete realization of standard accretion disk theory to date. Thus, they are well suited for both testing the theory's applicability to observed systems and for constraining properties of the black holes, including their spins.
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UNVERDICTED 2representative citing papers
Acoustic horizons in spinning black-hole accretion with spatially varying adiabatic index have surface gravities that depend on the black-hole spin parameter.
citing papers explorer
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Are most detected tidal disruption events partial?
SPH simulations of zero-energy partial TDEs find fallback ~t^{-9/4}, optical luminosities 10^{42-44} erg/s at 10^4 K and radii 10-100 au, indicating many detected TDEs may be partial rather than full.
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On the spin dependence of the emergent gravity phenomena as observed in axially symmetric black hole accretion with spatially varying adiabatic index
Acoustic horizons in spinning black-hole accretion with spatially varying adiabatic index have surface gravities that depend on the black-hole spin parameter.