1/2, 1, and 3/2--Law Non-Radiative Accretion Flows

Understand

Assuming self-similarity of the first kind, we get three possible values p=1/2, 1, 3/2 for the exponent describing the density profile, rho r^{-p}, of a non-radiative (and hence quasi-spherical) accretion flow.

• The high and low p cases are known as Bondi and Convection-Dominated accretion flows.
• The 1-law flow we tentatively identify with the so-called Magnetically-Frustrated accretion flow.
• If our interpretation is correct, the accretion flow must be, roughly speaking, a collection of Prandtl's turbulent jets.