SUMMARY
The inner radius of an accretion disc is primarily defined by the marginally stable orbit, which is 6M for a static black hole and reduces to 1M for a maximal Kerr black hole (where a/M=1). This conclusion is supported by various studies, although there is ongoing debate regarding the influence of the accretion disk's properties on this radius. Key references include works by Ken-ya Watarai, Xinwu Cao, and Kristen Menou, which provide further insights into the dynamics of accretion discs.
PREREQUISITES
- Understanding of black hole physics, specifically static and Kerr black holes.
- Familiarity with the concept of marginally stable orbits in astrophysics.
- Knowledge of accretion disk dynamics and their radiation properties.
- Basic comprehension of astrophysical research methodologies and literature.
NEXT STEPS
- Research "Kerr black hole properties" to understand the implications of a/M=1.
- Study "marginally stable orbits" in the context of accretion disks.
- Explore "radiation properties of accretion disks" to grasp their effects on inner radius determination.
- Read "Black Hole Accretion Disks On The Edge" by Kristen Menou for advanced insights.
USEFUL FOR
Astronomers, astrophysicists, and students studying black hole dynamics and accretion processes will benefit from this discussion.