2.1 Observational and Theoretical Evidence for the Accretion Paradigm
There is both observational and theoretical evidence for this picture. Based on optical spectra of AGN, Jackson & Wall (1999) identify two classes of object: Class A (quasars, ``N'' radio galaxies, Seyfert galaxies) with strong narrow emission lines and Class B (most radio galaxies and weak radio cores) with weak or no narrow line emission. Narrow line strength is considered a better parameter than, for example, broad line strength, as it is less affected by orientation effects (see, e.g., Antonucci & Miller 1985). In this scheme Class A objects are identified with high nuclear gas content and, therefore, with high accretion rate, while Class B AGN are identified with low accretion rate. An important point noted by Jackson & Wall is that the Fanaroff & Riley Class I radio sources are an homogeneous class, while FR II sources are not: FR Is are all Class B AGN while most, but not all, FR IIs are Class A. That is, some FR II sources appear to have powerful jets and yet a rather low accretion rate.
In addition, in present theories of accretion, a rapidly-accreting supermassive black hole embedded in an elliptical bulge of stars is predicted to appear as a quasar-like object (1-2 orders of magnitude brighter than its host). For 0.1 the standard disk models of Shakura & Sunyaev (1973) appear to be most appropriate, with the optical luminosity (integrated disk emission from plasma at a temperature of < 105 K) scaling in solar units as
If the black hole mass is directly related to galactic bulge luminosity,
i.e., Loptgal
2.4 x 1010
L
m90.8, as suggested by
Kormendy & Richstone
(1995),
then the ratio of accretion disk to bulge luminosity is
for > 0.1. On the other hand, a
drop in accretion rate well below this
value produces a much fainter ``advection-dominated''
(Narayan et al. 1998)
accretion disk with bolometric luminosity dropping as
Lbolacc
2, and
optical luminosity dropping even faster than that. (The exact accretion
rate at which
this drop-off occurs [cr ~
2] varies steeply with
the value
of the viscosity parameter ,
which is usually taken to be ~ 0.3 for ADAF models.)
Such disks are geometrically thick, optically
thin, and emit mainly nonthermal radio emission. For the remainder of this
paper, we will take = 0.1 to be
typical of Class A quasar-like objects
and = 0.01 to be typical of
Class B radio cores.