Powerful radiative jets in supercritical accretion discs around non-spinning black holes

摘要: We describe a set of simulations super-critical accretion onto non-rotating supermassive BH. The flow is radiation pressure dominated and takes the form geometrically thick disk with twin low-density funnels around rotation axis. For rates $\gtrsim 10 \dot M_{\rm Edd}$, there sufficient gas in funnel to make this region optically thick. Radiation from first flows into funnel, after which it accelerates along resulting jet baryon-loaded has terminal density-weighted velocity $\approx 0.3c$. Much radiative luminosity converted kinetic energy by time escaping becomes thin. an observer viewing down axis, isotropic equivalent total as much $10^{48}\,\rm erg\,s^{-1}$ for $10^7 M_\odot$ BH accreting at $10^3$ Eddington. Therefore, energetically, simulated jets are consistent observations most powerful tidal disruption events, e.g., Swift J1644. is, however, too low match Lorentz factor $\gamma > 2$ inferred There no such conflict case other events. Since favorably oriented observers see luminosities that highly super-Eddington, models can explain ultra-luminous X-ray sources, least terms energetics, without requiring intermediate mass black holes. Finally, since have mildly relativistic velocities, they well observed SS433. latter are, more collimated than jets. This suggests that, even if magnetic fields not important acceleration, may perhaps still play role confining jet.