Accretion phenomena and theories

The Eddington Luminosity
M
• A limit to which luminosity can be produced by a
given object, assuming a steady accretion state.
• The inward gravitational force on matter is balanced
by the outward transfer of momentum by radiation.
• At this point accretion stops, effectively imposing a
‘limit’ on the luminosity of a given body.
r
Electrostatic forces
between e - and p binds
them so act as a pair
m F grav =GMm/r 2 where m=m p +m e ~ m p
F grav F rad
= Lσ T /(4πr 2 c)
F rad = [L/(4πr 2 hν)]σ T (hν/c)
F grav = F rad the Eddington luminosity
L= 4πcGMm/σ T
=1.3 x10 38 (M/M sun ) ergs/s