Predrag Jovanović and Luka Č. PopovićAstronomical ObservatoryBelgrade, Serbia
Outline Supermassive black holes (SMBHs) in nuclei ofactive galaxies X-ray emission from relativistic accretion disksaro...
Black holes in nature classification according to the metric:1. Schwarzschild (non-rotating and uncharged)2. Kerr (rotati...
SMBHs in Active Galaxies Small very bright coreembedded in an otherwisetypical galaxyLeft: NGC 5548 (Seyfert galaxy)Right...
Armitage, P. J., Reynolds, C. S. 2003, MNRAS, 341, 1041
Fabian, A. C. 2006, AN, 327, 943The broad Fe Kα spectral lineTanaka et al, 1995, Nature, 375, 659 broad emission spectral...
Supermassive black hole binaries (SMBHBs)
 in units where horizon of BH: radius of marginally stable orbit: Two approaches:1. integrating the null geodesic equa...
• Surface emissivity of the disk:0( ) qr r  • Total observed flux:40( ) ( ) ( ) ,obs obs obsimageF E r g E gE d   ...
ResultsJovanović & Popović, 2008,Fortschr. Phys. 56, 456
Modeled Fe Kα spectral line profiles for several values of angular momentumparameter a, and for inclination angle i = 20º ...
The broad Fe Kα line from SMBHBs
Keplerian radial velocity curves of SMBHBs  1,21,21,2 1,2 1 1 2 222 sincos cos , ,1rada iV K e K M a M aP e     ...
Composite Fe Kα line profiles ICase II: q = 0.5, a = 0.01 pc, i = 60o, e = 0.5 and ω = 90oCase I: q = 0.5, a = 0.01 pc, i ...
Composite Fe Kα line profiles IICase IV: q = 1.0, a = 0.05 pc, i = 60o, e = 0.5 and ω = 90oCase III: q = 1.0, a = 0.01 pc,...
Influence of SMBHBson optical linesBon et al. 2012, ApJ, 759, 118Popović, 2012, NewAR, 56, 74
Conclusions1. We developed and performed simulations of the X-ray radiation fromrelativistic accretion disks around single...
Jovanović P., Popović L. Č., 2009, chapter in book “Black Holes and Galaxy Formation”,Nova Science Publishers Inc, Hauppau...
P. Jovanović: Supermassive Binary Black Hole - Possible Observational Effects in the X-ray Emission
Upcoming SlideShare
Loading in …5
×

P. Jovanović: Supermassive Binary Black Hole - Possible Observational Effects in the X-ray Emission

545 views

Published on

Balkan Workshop BW2013
Beyond the Standard Models
25 – 29 April, 2013, Vrnjačka Banja, Serbia

Published in: Education, Technology
0 Comments
0 Likes
Statistics
Notes
  • Be the first to comment

  • Be the first to like this

No Downloads
Views
Total views
545
On SlideShare
0
From Embeds
0
Number of Embeds
39
Actions
Shares
0
Downloads
0
Comments
0
Likes
0
Embeds 0
No embeds

No notes for slide

P. Jovanović: Supermassive Binary Black Hole - Possible Observational Effects in the X-ray Emission

  1. 1. Predrag Jovanović and Luka Č. PopovićAstronomical ObservatoryBelgrade, Serbia
  2. 2. Outline Supermassive black holes (SMBHs) in nuclei ofactive galaxies X-ray emission from relativistic accretion disksaround SMBHs: the broad Fe Kα spectral line Supermassive black hole binaries (SMBHBs) Our investigations: applications of ray-tracing inKerr metric for simulations of the Fe Kα line, emittedfrom accretion disks of SMBHs and SMBHBs Conclusions
  3. 3. Black holes in nature classification according to the metric:1. Schwarzschild (non-rotating and uncharged)2. Kerr (rotating and uncharged)3. Reissner–Nordström (non-rotating and charged)4. Kerr–Newman (rotating and charged) classification according to their masses:1. Mini, micro or quantum mechanical: MBH  M (primordialblack holes in the early universe)2. stellar-mass: MBH < 102 M (in the X-ray binary systems)3. intermediate-mass: MBH  102 − 105 M (in the centers ofglobular clusters)4. supermassive: MBH  105 − 1010 M (in the centers of allgalaxies, including ours)
  4. 4. SMBHs in Active Galaxies Small very bright coreembedded in an otherwisetypical galaxyLeft: NGC 5548 (Seyfert galaxy)Right: NGC 3277 (regular galaxy)
  5. 5. Armitage, P. J., Reynolds, C. S. 2003, MNRAS, 341, 1041
  6. 6. Fabian, A. C. 2006, AN, 327, 943The broad Fe Kα spectral lineTanaka et al, 1995, Nature, 375, 659 broad emission spectral line at 6.4 keV asymetric profile with narrow brightblue peak and wide faint red peak Line width corresponds to velocity:v ~ 100.000 km/s (MCG-6-30-15)v ~ 48.000 km/s (MCG-5-23-16)v ~ 20000 – 30000 km/s (many other)
  7. 7. Supermassive black hole binaries (SMBHBs)
  8. 8.  in units where horizon of BH: radius of marginally stable orbit: Two approaches:1. integrating the null geodesic equations starting from a giveninitial position in the disk to the observer at infinity2. tracing rays following the trajectories from the sky plane to thedisk: only those photon trajectories that reach observers skyplane are consideredOur investigations: ray-tracing in Kerr metric
  9. 9. • Surface emissivity of the disk:0( ) qr r  • Total observed flux:40( ) ( ) ( ) ,obs obs obsimageF E r g E gE d    obsemg
  10. 10. ResultsJovanović & Popović, 2008,Fortschr. Phys. 56, 456
  11. 11. Modeled Fe Kα spectral line profiles for several values of angular momentumparameter a, and for inclination angle i = 20º (left) and i = 40º (right)Jovanović, BorkaJovanović, Borka, 2011, BalticObservations of the Fe Kα line in thecase of the nucleus of Cygnus A (3C405) (black crosses with error bars)observed by Chandra, and thecorresponding simulated profiles for 4different values of black hole spin(solid color lines).
  12. 12. The broad Fe Kα line from SMBHBs
  13. 13. Keplerian radial velocity curves of SMBHBs  1,21,21,2 1,2 1 1 2 222 sincos cos , ,1rada iV K e K M a M aP e            2 321 21 24,aP a a aG M M  Keplerian radial velocity curves forand the following orbital elements:a = 0.01 pc, i = 60o, e = 0.75 and ω = 90o81 1 10 ,M M  72 5 10M M   2 1/ 0.5 , 0q M M   • K1,2 – semiaplitudes of thevelocity curves,• γ – systemic velocity
  14. 14. Composite Fe Kα line profiles ICase II: q = 0.5, a = 0.01 pc, i = 60o, e = 0.5 and ω = 90oCase I: q = 0.5, a = 0.01 pc, i = 30o, e = 0 and ω = 90o
  15. 15. Composite Fe Kα line profiles IICase IV: q = 1.0, a = 0.05 pc, i = 60o, e = 0.5 and ω = 90oCase III: q = 1.0, a = 0.01 pc, i = 60o, e = 0.75 and ω = 90o
  16. 16. Influence of SMBHBson optical linesBon et al. 2012, ApJ, 759, 118Popović, 2012, NewAR, 56, 74
  17. 17. Conclusions1. We developed and performed simulations of the X-ray radiation fromrelativistic accretion disks around single and binary SMBHs, based on ray-tracing method in Kerr metric2. These simulations enables us to study space-time geometry in vicinity ofsuch SMBHs, their properties, strong gravity effects and accretion physics3. If detected, the unusual, complex and shifted composite Fe Kα line profilescould provide evidence about presence of the binary SMBH systems4. Such complex Fe Kα line profiles could be used for studying the parametersand orbits of SMHBs, especially in the cases when they are composed fromtwo very different constituent line profiles (e.g. when one of them issignificantly wider)5. This is the case when primary and secondary SMBHs have differentproperties and/or their accretion disks have different parameters (such asinner and outer radii and/or emissivity)
  18. 18. Jovanović P., Popović L. Č., 2009, chapter in book “Black Holes and Galaxy Formation”,Nova Science Publishers Inc, Hauppauge NY, USA, 249-294, arXiv:0903.0978Reviews of our results

×