Radiatively-Driven Relativistic Accretion Disk Winds

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We theoretically examined relativistic disk winds driven by disk radiation fields. For the present purpose, we quantitatively caluculated the full components of radiation fields produced by a standard accretion disk around Schwarzschild and extreme Kerr black holes, under the pseudo-Newtonian gravity and special relativity. The typical strength of radiation fields of disks around the Schwarzschild hole reduces by about 50%, whereas that around the extreme Kerr hole increases by about ten times, as compared with the Newtonian case. We found that the wind is easy to blow off from the disk around the Kerr hole, although it becomes difficult from the disk around the Schwarzschild hole, as long as the accretion rate is subcritical. In the extreme Kerr case the maximum terminal speed is about 0.5c for the critical accretion rate.

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