Study of Advective Energy Transport in the Inflow and Outflow of Super-Eddington Accretion Flows

Abstract

Photon trapping is believed to be an important mechanism in super-Eddington accretion, which greatly reduces the radiative efficiency as photons are swallowed by the central black hole before they can escape from the accretion flow. This effect is interpreted as the radial advection of energy in one-dimensional height-integrated models, such as the slim-disk model. However, when multidimensional effects are considered, the conventional understanding may no longer hold. In this paper, we study the advective energy transport in super-Eddington accretion based on a new two-dimensional inflow–outflow solution with radial self-similarity, in which the advective factor is calculated self-consistently by incorporating the calculation of radiative flux instead of being set as an input parameter. We found that radial advection is actually a heating mechanism in the inflow due to compression, and the energy balance in the inflow is maintained by cooling via radiation and vertical (θ-direction) advection, which transports entropy upward to be radiated closer to the surface or carried away by the outflow. As a result, fewer photons are advected inward, and more photons are released from the surface, so that the mean advective factor is smaller and the emergent flux is higher than the fluxes predicted by the slim-disk model. The radiative efficiency of super-Eddington accretion thus should be higher than that of the slim-disk model, which agrees with the results of some recent numerical simulations.

Super-Eddington Magnetized Neutron Star Accretion Flows: A Self-similar Analysis

“…Although the resulting self-similar solution can conveniently provide the disk properties under given initial conditions, they should be regarded as approximations. In reality, the analytical solution for the disks should incorporate a three-dimensional or at least two-dimensional structure and discard the vertical force balance assumption, as the formation of disk winds indicates the dynamic nature of the vertical gas; only by constructing a stratified disk structure can we better predict the properties of the disk wind and inflow (e.g., Cao & Gu 2022;Jiao 2023).…”