Origins, Structure, and Inflows of m=1 Modes in Quasi-Keplerian Disks

Understand

Simulations show eccentric disks (m=1 modes) forming around quasi-Keplerian potentials, a topic of interest for fueling quasars, forming super-massive BHs, planet formation and migration, explaining the origin and properties of nuclear eccentric stellar disks like that in M31, and driving the formation of the obscuring AGN torus.

• We consider the global, linear normal m=1 modes in collisionless disks, without the restriction that the disk mass be negligible relative to the central (Keplerian) mass.
• We derive their structure and key resonance features, and show how they arise, propagate inwards, and drive both inflow/outflow and eccentricities in the disk.
• We compare with hydrodynamic simulations of such disks around a super-massive BH, with star formation, gas cooling, and feedback.