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Black Holes in Xi`an

Black Holes in Xi`an. Black holes Accretion disks Jets Winds and outflows 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. 10 11 erg/sec. M. Bentz.

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Black Holes in Xi`an

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  1. Black Holes in Xi`an • Black holes • Accretion disks • Jets • Winds and outflows • The broad line region

  2. My Stamp Collection

  3. My Stamp Collection

  4. Black hole stamp

  5. Black hole stamp Shai Kaspi The industry Brad Peterson

  6. Fireworks in Xi`an 1 cm 1011 erg/sec M. Bentz

  7. BH Mass Functions Greene & Ho in prep Jenny Greene

  8. 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

  9. The Fundamental Plane Relationship of Astrophysical Black Holes Ran Wang Alessandro Marconi

  10. Can this be generalized to AGN?

  11. Accretion disk stamp Omer Blaes It is all magnetically driven Please Omer Will you give us back our corona? The X-ray astronomers

  12. Undressing 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

  13. Relativistic disk lines Tahir 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 5 5.25 5.5 5.75 6 6.3 keV Jane Turner Relativistic narrow lines are common and VERY strong ! 40 80 120 160 200 eV

  14. X-ray variability

  15. Characteristic time-scales scale with black hole mass – Phil Uttley >108 M 106 M 4107 M

  16. Jet stamp Wagner Boettecher Maraschi New opportunity

  17. 0 Blazar Models Proton-induced radiation mechanisms: Injection, acceleration of ultrarelativistic electrons and protons Relativistic jet outflow with G ≈ 10 nFn g-q Qe,p (g,t) n g1 g2 g Synchrotron emission of primary e- Hadronic Models nFn n

  18. Chairman Wang said

  19. Major questions Jian-Min Wang 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? jet formation is BH mass-scale free? jet component? jet interaction with surrounding photons from disk, BLR? Binary BH in OJ 287? See several posters

  20. Winds and Outflows stamp But: Mike Brotherton does not like some of it … X-ray Ultraviolet Mid-Infrared Gallagher 2006

  21. vmax vs. Daox te~1 Daox

  22. Emission-Line Profiles at Low Flux Levels Mike Crenshaw

  23. Simple Geometric Model • r = 0.1 pc,  = 45, vr = vlos = - 490 km s-1 • Assume v = 0, then v = vT = 2100 km s-1(vT = 10,000 km s-1 also shown)

  24. 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.

  25. More winds • M. Guainazzi – WA is also warm reflector (but 200 pc large) • F. Nicastro – WA is <0.1 pc in size • Goncalves – He-like X-ray lines are good wind diagnostics

  26. Broad Line Region stamp • Joe Shields • What is the physical origin of the Baldwin effect (29 years is not enough..) • M. Joly • What is the origin of the extremely strong FeII lines (26 years is not enough ..)

  27. Ari Laor - Why does RBLRL1/2? Theory Netzer & Laor (1993) Σion=1023U, U=nγ/ne Dust suppression of line emission. Dust= Σ/1021=100U Line suppression for U>0.01 Dust sublimation. Rsub≤0.2L461/2 pc BLR is dust bounded BLR IR cont’ NLR Lines 1021 Dusty gas IR 1022 Inevitable & no free parameters

  28. 2D 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). Echo image Ech Velocity-delay map Kollatschny 2003a • HeII lines are gravitationally shifted • OVII is also gravitationally shifted at r=20rs 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

  29. More BLR goodies • B. Welsh: BLR gas is falling in (??) • I. Strateva: double-peaked line profiles • F. Hamann: BLR metallicity goes with BH mass (but … L/L(Edd) and time dependence) • The SDSS industry (or: what can we learn by studying large samples?) - Nagao

  30. Black holes Accretion disk Winds and outflows Jets BLR Dr. Joe Shields Xi`an, China

  31. October 21 2006 Dear Joe, Please review for us the other sessions Thanks…..

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