Black Holes in Xi`an Black holes Accretion disks Jets Winds and outflows The broad line region.
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Transcript of Black Holes in Xi`an Black holes Accretion disks Jets Winds and outflows The broad line region.
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Black Holes in Xi`anBlack Holes in Xi`an
Black holesBlack holes Accretion disksAccretion disks JetsJets Winds and outflowsWinds and outflows The broad line regionThe broad line region
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My Stamp CollectionMy Stamp Collection
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My Stamp CollectionMy Stamp Collection
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Black hole stampBlack hole stamp
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Shai Kaspi
Black hole stamp
Brad Peterson
The industry
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1011 erg/sec
1 cm
Fireworks in Xi`an
M. Bentz
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BH Mass FunctionsBH Mass Functions
Greene & Ho in prep
Jenny Greene
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L/LL/LEddEdd vs. redshift vs. redshift
Accretion rate increases with z for all mass BHs
See also very interesting result by Y.M. Chen et al about duty cycle
M=107.6
M=108.6
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The Fundamental Plane The Fundamental Plane Relationship of Astrophysical Relationship of Astrophysical
Black HolesBlack Holes
The Fundamental Plane The Fundamental Plane Relationship of Astrophysical Relationship of Astrophysical
Black HolesBlack Holes
Ran WangRan Wang
Alessandro MarconiAlessandro MarconiRan WangRan Wang
Alessandro MarconiAlessandro Marconi
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MMBHBH-L-LMMBHBH--σσMMBHBH-M-MvirvirMMBHBH-W-Wgravgrav
ObservedObservedFundameFundame
ntalntal
1.1±0.11.1±0.10.350.35
±0.05±0.05
4.04.0 ±0.3±0.30.250.25
±0.05±0.05
1.01.0 ±0.1±0.10.270.27
±0.05±0.05
0.70.7 ±0.1±0.10.220.22 ±0.03±0.03
MMBHBH-L-L 1.11.10.250.25
2.62.60.350.35
0.870.870.280.28
0.560.560.290.29
MMBHBH--σσ1.021.020.380.38
4.04.00.250.25
0.950.950.330.33
0.690.690.290.29
MMBHBH-M-Mvirvir1.141.140.280.28
3.183.180.320.32
1.01.00.250.25
0.660.660.260.26
MMBHBH-W-Wgravgrav1.321.320.320.32
4.144.140.300.30
1.181.180.270.27
0.70.70.250.25
Can this be generalized to AGN?
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Omer Blaes
Accretion disk stamp
Please Omer
Will you give us back our corona?
The X-ray astronomers
It is all magnetically driven
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Undressing AGNsUndressing AGNs
Why is this different from Seyfert 1s (Paulina Lira)?
Can the BLR provide the mysterious screen?
Covering=0.1
Column density=1023cm-2
Scattering probability=0.01
See also poster
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00.5
11.5
22.5
33.5
44.5
5
Observed Energy
5 5.25 5.5 5.75 6 6.3 keV
0
0.5
1
1.5
2
2.5
3
3.5
4
EW eV
40 80 120 160 200 eV
Relativistic disk linesRelativistic disk linesTahir Yaqoob
1. 25-50% of all AGNs show relativistic disk lines - ???
2. We are trying hard but so far have not succeeded in measuring black hole spin
Jane Turner
Relativistic narrow lines are common and VERY strong !
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X-ray variabilityX-ray variability
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Characteristic time-scales scale Characteristic time-scales scale with black hole mass – Phil Uttleywith black hole mass – Phil Uttley
>108 M 4107 M 106 M
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Jet stamp
Wagner
Boettecher
Maraschi
New opportunity
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Blazar ModelsBlazar ModelsRelativistic jet outflow with ≈ 10
Injection, acceleration of ultrarelativistic electrons and
protons
Qe
,p (,
t)
Synchrotron emission of primary e-
F
Proton-induced radiation
mechanisms:
F
-q
Hadronic Models
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Chairman Wang saidChairman Wang said
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Major questionsMajor questions
jet formation/ejection from diskjet formation/ejection from disk : : are they really connectedare they really connected??
how to form and quenchhow to form and quench?? how to accelerate jetshow to accelerate jets??
jet fraction of the energyjet fraction of the energy output from BH accretionoutput from BH accretion??
jet formation is BH mass-scale freejet formation is BH mass-scale free??
jet componentjet component??jet interaction with surrounding photons from disk, jet interaction with surrounding photons from disk, BLRBLR??
Jian-Min Wang
Binary BH in OJ 287?
See several posters
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Ultraviolet
X-ray
Mid-Infrared
Gallagher 2006
But:
Mike Brotherton does not like some of it …
Winds and Outflows stamp
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vvmax max vs. vs. oxox
oxox
ee~~11
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Emission-Line Profiles at Low Flux Levels
Mike Crenshaw
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Simple Geometric Model
r = 0.1 pc, r = 0.1 pc, = 45 = 45, v, vrr = v = vloslos = - 490 km s = - 490 km s-1-1
Assume Assume vv = 0, then = 0, then vv = = vvT T = 2100 km s= 2100 km s-1-1 (v(vTT = 10,000 km s = 10,000 km s-1-1 also also
shown)shown)
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Doron Chelouche
Do we really need that level of sophistication?(the case of stellar winds)
•Asymmetric UV emission lines
•Symmetric X-ray lines
Owocki et al.
KK LL
MM
1.0
0.1
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More windsMore winds
M. Guainazzi – WA is also warm M. Guainazzi – WA is also warm reflector (but 200 pc large)reflector (but 200 pc large)
F. Nicastro – WA is <0.1 pc in sizeF. Nicastro – WA is <0.1 pc in size Goncalves – He-like X-ray lines are Goncalves – He-like X-ray lines are
good wind diagnosticsgood wind diagnostics
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Broad Line Region stampBroad Line Region stamp
Joe ShieldsJoe Shields– What is the physical origin What is the physical origin
of the Baldwin effect (29 of the Baldwin effect (29 years is not enough..)years is not enough..)
M. JolyM. Joly– What is the origin of the What is the origin of the
extremely strong FeII lines extremely strong FeII lines (26 years is not enough ..)(26 years is not enough ..)
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Ari Laor - Why does Ari Laor - Why does RRBLRBLR LL1/21/2 ??
Dust suppression of line emission.
Theory Netzer & Laor (1993)
BLR IR cont’ NLR
Σion=1023U, U=nγ/ne
IRLines
Dusty gas
Dust= Σ/1021=100U
Line suppression for U>0.01
Dust sublimation.
Rsub≤0.2L461/2 pc
BLR is dust bounded
Inevitable & no free parameters
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2D Transfer Function - W. Kollatschny2D Transfer Function - W. Kollatschny
2-D CCF : correlation of Hβ line profile segments with cont. variations (grey scale)
Contours of correlation coefficient at levels of .85 to .925 (solid lines).
Dashed curves: theoretical escape velocity envelopes for masses of 0.5, 1., 2. 107 MO (from bottom to top).
Kollatschny 2003a
Theoretical velocity-delay maps for different flows: Keplerian disk BLR model: fast response of both outer line wings
Welsh & Horne 1991, Horne et al. 2004
Velocity-delay map
E
c
h
Echo image
HeII lines are gravitationally shifted
OVII is also gravitationally shifted at r=20rs
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More BLR goodiesMore BLR goodies
B. Welsh: BLR gas is falling in (??)B. Welsh: BLR gas is falling in (??) I. Strateva: double-peaked line profilesI. Strateva: double-peaked line profiles F. Hamann: BLR metallicity goes with BH F. Hamann: BLR metallicity goes with BH
mass (but … L/L(Edd) and time mass (but … L/L(Edd) and time dependence)dependence)
The SDSS industry (or: what can we learn The SDSS industry (or: what can we learn by studying large samples?) - Nagaoby studying large samples?) - Nagao
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Black holes
Accretion disk
Jets
Winds and outflows
BLR
Dr. Joe Shields
Xi`an, China
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Dear Joe,
Please review for us the other sessions
Thanks …..
October 21 2006