Black Holes in Xian u Black holes u
Black Holes in Xi`an u Black holes u Accretion disks u Jets u Winds and outflows u The broad line region
My Stamp Collection
My Stamp Collection
Black hole stamp
Black hole stamp Shai Kaspi The industry Brad Peterson
Fireworks in Xi`an 1 cm 1011 erg/sec M. Bentz
BH Mass Functions Greene & Ho in prep Jenny Greene
L/LEdd vs. redshift M=107. 6 M=108. 6 Accretion rate increases with z for all mass BHs See also very interesting result by Y. M. Chen et al about duty cycle
The Fundamental Plane Relationship of Astrophysical Black Holes Ran Wang Alessandro Marconi
MBH-L MBH-σ MBH-Mvir MBH-Wgrav Observed 1. 1± 0. 1 4. 0 ± 0. 3 Fundament 0. 35 ± 0. 05 0. 25 ± 0. 05 al 1. 0 ± 0. 1 0. 27 ± 0. 05 0. 7 ± 0. 1 0. 22 ± 0. 03 MBH-L 1. 1 0. 25 2. 6 0. 35 0. 87 0. 28 0. 56 0. 29 MBH-σ 1. 02 0. 38 4. 0 0. 25 0. 95 0. 33 0. 69 0. 29 MBH-Mvir 1. 14 0. 28 3. 18 0. 32 1. 0 0. 25 0. 66 0. 26 MBHWgrav 1. 32 0. 32 4. 14 0. 30 1. 18 0. 27 0. 25 Can this be generalized to AGN?
Accretion disk stamp Omer Blaes It is all magnetically driven Please Omer Will you give us back our corona? The X-ray astronomers
Undressing AGNs Why is this different from Seyfert 1 s (Paulina Lira)? Can the BLR provide the mysterious screen? Covering=0. 1 Column density=1023 cm-2 Scattering probability=0. 01 See also poster
Relativistic disk lines Tahir Yaqoob 1. 25 -50% of all AGNs show relativistic disk lines - ? ? ? 5 5. 25 5. 75 6 6. 3 ke. V 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 ! 40 80 120 160 200 e. V
X-ray variability
Characteristic time-scales scale with black hole mass – Phil Uttley >108 M 4 107 M 106 M
Jet stamp Wagner Boettecher Maraschi New opportunity
Relativistic jet outflow with G ≈ 10 g-q g 1 Proton-induced radiation mechanisms: n. Fn Qe, p (g, t) Injection, acceleration of ultrarelativistic electrons and protons Blazar Models n g 2 g n. Fn Synchrotron emission of primary e- n Hadronic Models
Chairman Wang said
Jian-Min Wang Major questions jet formation/ejection from disk: are they really connected? how to form and quench? how to accelerate jets? jet fraction of the energy output from BH accretion? Binary BH in OJ 287? See several posters jet formation is BH mass-scale free? jet component? jet interaction with surrounding photons from disk, BLR?
Winds and Outflows stamp Xra But: y Ult r av iol et Mi d-I nfr Mike Brotherton does not like some of it … are d Gallagher 2006
vmax vs. Daox t e ~1 Daox
Emission-Line Profiles at Low Flux Levels Mike Crenshaw
Simple Geometric Model r = 0. 1 pc, = 45 , vr = vlos = - 490 km s-1 u Assume v = 0, then v = v. T = 2100 km s-1 (v. T = u 10, 000 km s-1 also shown)
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.
More winds u M. Guainazzi – WA is also warm reflector (but 200 pc large) u F. Nicastro – WA is <0. 1 pc in size u Goncalves – He-like X-ray lines are good wind diagnostics
Broad Line Region stamp u Joe Shields – What is the physical origin of the Baldwin effect (29 years is not enough. . ) u M. Joly – What is the origin of the extremely strong Fe. II lines (26 years is not enough. . )
Ari Laor - Why does RBLR L 1/2 Theory ? Netzer & Laor (1993) Dust suppression of line emission. Σion=1023 U, U=nγ/ne Dust= Σ/1021=100 U Line suppression for U>0. 01 Dust sublimation. Rsub≤ 0. 2 L 461/2 pc BLR is dust bounded 1021 1022 Lines IR D ty s u s ga BLR IR cont’ NLR Inevitable & no free parameters
2 D 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). Velocity-delay map Kollatschny 2003 a E Echo image c h Theoretical velocity-delay for different flows: He. II lines aremaps gravitationally shifted Keplerian disk BLR model: fast response of both outer line wings OVII is also gravitationally shifted at Welsh & Horne 1991, Horne et al. 2004 r=20 rs
More BLR goodies B. Welsh: BLR gas is falling in (? ? ) u I. Strateva: double-peaked line profiles u F. Hamann: BLR metallicity goes with BH mass (but … L/L(Edd) and time dependence) u The SDSS industry (or: what can we learn by studying large samples? ) - Nagao u
Accretion disk Dr. Joe Shields Black holes Winds and outflows Xi`an, China Jets BLR
October 21 2006 Dear Joe, Please review for us the other sessions Thanks …. .
- Slides: 32