Hi tiny-tim
In most cases, the inner edge of the accretion disk is considered to coincide with the marginally stable which is 6M for a static black hole, reducing to 1M for a maximal Kerr
black hole where a/M=1, though there seems to be some debate that the properties of the accretion disk itself can have an effect on this-
A couple of links-
'Where is a Marginally Stable Orbit in Luminous Accretion Disk' by Ken-ya Watarai Watarai, Shin Mineshige
http://quasar.cc.osaka-kyoiku.ac.jp/...Poster2004.pdf
'The radiation properties of an accretion disk with a non-zero
torque on its inner edge' by Xinwu Cao, Y.D. Xu
http://arxiv.org/abs/astro-ph/0211220
'Black Hole Accretion Disks On The Edge' by Kristen Menou
http://arxiv.org/abs/astro-ph/0304421