Critical Accretion Disk

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For a supercritical accretion regime, we propose a critical accretion disk, where the mass-accretion rate is regulated just at the critical rate with the help of wind mass-loss. We first derive a critical radius, inside of which the standard picture is violated, using the condition that the radiative force is balanced by the gravity in the vertical direction. The critical radius r_(cr) is found to be r_(cr) =(9sqrt(3)sigma_T/16(pi)cm_p)M_(input) =1.95(M_(input)/M_(crit))r_g , where M_(input) is the mass-accretion rate at the outer edge of the disk, M_(crit) the critical accretion rate, and r_g the Schwarzschild radius of the central object. Outside of this critical radius, the disk is in a radiation-pressure dominated standard state, while inside this radius the disk is in a critical state, where the excess mass is expelled by wind and the accretion rate is kept to be just at the critical rate at any radius inside r_(cr). In such a critical accretion disk, the disk thickness is H ～ (1/6sqrt3)_r and the surface temperature is sigmaT^4 ～ (2/3sqrt3)L_E/4(pi)r^2 , where L_E is the Eddington luminosity. The total disk luminosity becomes L_(disk) ～ (2/3sqrt3)[In(r_(cr)/r_(in)) + l]L_E, where r_(in) is the inner radius. We apply the present model to microquasars and narrow-line Seyfert 1 galaxies, which are supposed to be under supercritical accretion.

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