Slide 19
Slide 19 text
n thin disks, most of the mass
e radii reaches the central black
, in thick disks, very little of the
nds up accreting into the hole.
the mass circulates in convective
or is driven away in an unbound
6). This in turn causes the
tion from the accretion flow to
ally. Because the fate of sup-
pends so strongly on the mode
hin versus thick), it is likely
reting black holes occupy a
velope
Main disk body
KDP
30
20
10
10
20
0
–10
1
SNE, GRB
Radiation–trapped
Bright XRBs, AGN
Faint XRBs, AGN
2
2 3
log R (RS
)
log R (km)
log M (MEdd
)
log M (g s–1)
Regimes
of BH
accretion
Super-Eddington,
radiation-trapped
TDE, AGN?
Near-Eddington
Sub-Eddington
retion flow to
e fate of sup-
on the mode
), it is likely
es occupy a
disk body
KDP
30
20
10
0
SNE, GRB
Radiation–trapped
Bright XRBs, AGN
Faint XRBs, AGN
log M (MEdd
)
log M (g s–1)
dy
DP
20
10
0
–10
1
Radiation–trapped
Bright XRBs, AGN
Faint XRBs, AGN
2
log R (RS
)
log M (MEdd
)
log M (g s–1)
black
of the
e hole.
vective
bound
es the
low to
f sup-
mode
likely
upy a
DP
30
10
20
SNE, GRB
Radiation–trapped
2 3
log R (km)
log M (MEdd
)
log M (g s–1)
Narayan & Quataert 2005
Faint XRBs, low-
luminosity AGNs
Bright XRB, quasars, Seyferts
log R (pc)
-4 -5
?
?