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The inner region of a luminous accretion disk is radiation pressuredominated. We estimate the surface temperature of a radiation pressuredominated accretion disk, \Theta=(c_s/r\Omega_K)^2<<(H/r)^2, which issignificantly lower than that of a gas pressure dominated disk, \Theta (H/r)^2.This means that the outflow can be launched magnetically from the photosphereof the radiation pressure dominate disk only if the effective potential barrieralong the magnetic field line is extremely shallow or no potential barrier ispresent. For the latter case, the slow sonic point in the outflow may probablybe in the disk, which leads to a slow circular dense flow above the disk. Thisimplies that hot gas (probably in the corona) is necessary for launching a jetfrom the radiation pressure dominated disk, which provides a naturalexplanation on the observational evidence that the relativistic jets arerelated to hot plasma in some X-ray binaries and active galactic nuclei. Weinvestigate the outflows accelerated from the hot corona above the disk by themagnetic field and radiation force of the accretion disk. We find that, withthe help of the radiation force, the mass loss rate in the outflow is high,which leads to a slow outflow. This may be the reason why the jets inradio-loud narrow-line Seyfert galaxies are in general mild relativisticcompared with those in blazars.

The outflows accelerated by the magnetic fields and radiation force of accretion disks