Super-Eddington growth of black holes in the early Universe: effects of disk radiation spectra

We investigate the properties of accretion flows on to a black hole (BH) with a mass of MBH embedded in an initially uniform gas cloud with a density of n(infinity) in order to study rapid growth of BHs in the early Universe. In previous work, the conditions required for super-Eddington accretion from outside the Bondi radius were studied by assuming that radiation produced at the vicinity of the central BH has a single power-law spectrum nu(-alpha) at h nu >= 13.6 eV(alpha similar to 1.5). However, radiation spectra surely depend on the BH mass and accretion rate, and determine the efficiency of radiative feedback. Here, we perform two-dimensional multifrequency radiation hydrodynamical simulations taking into account more realistic radiation spectra associated with the properties of nuclear accretion discs. We find that the critical density of gas surrounding the BH, above which transitions to super-Eddington accretion occur, is alleviated for a wide range of masses of seed BHs (10 less than or similar to M-BH/M-circle dot less than or similar to 10(6)) because photoionization for accretion disc spectra are less efficient than those for single power-law spectra with 1 less than or similar to alpha less than or similar to 3. For disc spectra, the transition to super-Eddington is more likely to occur for lower BH masses because the radiation spectra become too hard to ionize the gas. Even when accretion flows are exposed to anisotropic radiation, the effect due to radiation spectra shrinks the ionized region and likely leads to the transition to a wholly neutral accretion phase. Finally, by generalizing our simulation results, we construct a new analytical criterion required for super-Eddington accretion; (M-BH/10(5) M-circle dot)(n(infinity)/10(4) cm(-3)) greater than or similar to 2.4(/100 eV)(-5/9), where is the mean energy of ionizing radiation from the central BH.