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Disk-Jet Connection in the Radio Galaxies 3C 120 and 3C 111

Disk-Jet Connection in the Radio Galaxies 3C 120 and 3C 111. Ritaban Chatterjee NERQUAM 2010, May 18th, 2010. Data Sources. X-Ray (RXTE-PCA) and VLBA: A. Marscher, S. Jorstad (BU) 37 GHz : Anne Lahteenmaki, Merja Tornikoski, Talvikki Hovatta (Metsahovi Observatory, Finland).

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Disk-Jet Connection in the Radio Galaxies 3C 120 and 3C 111

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  1. Disk-Jet Connection in the Radio Galaxies 3C 120 and 3C 111 Ritaban Chatterjee NERQUAM 2010, May 18th, 2010.

  2. Data Sources • X-Ray (RXTE-PCA) and VLBA: A. Marscher, S. Jorstad(BU) • 37 GHz : Anne Lahteenmaki, Merja Tornikoski, Talvikki Hovatta(Metsahovi Observatory, Finland). • R Band: I. McHardy (U. Southampton), Kevin Marshall, H. Richard Miller, Wesley T. Ryle(Georgia State) • V Band: Large international team (please see ApJ paper for details) led by Martin Gaskell(U. Texas, Austin, U. Nebraska, Lincoln).

  3. AGN : Unified Picture Blazar BLRG 3C 120 and 3C 111 are BLRGs Courtesy: C.M. Urry & P. Padovani

  4. Mirabel & Rodriguez 1998, Nature,392, 673.

  5. OUTLINE • 3C 120, 3C 111: Characteristic timescale • 3C 120, 3C 111: Accretion disk-jet connection

  6. 3C 120 1. BLRG 2. FR-I 3. z=0.033 4. Angle between jet axis and line of sight ~20o 5 GHz Image: Walker, Benson & Unwin 1987 ApJ, 316, 546

  7. 3C 111 1. BLRG 2. FR-II 3. z=0.048 4. Angle between jet axis and line of sight ~20o 1.4 GHz Image: Linfield & Perley 1984, ApJ, 279, 60

  8. Variability at different timescales Power Spectral Density (PSD) => Amplitude of variability as a function of timescale

  9. X-Ray PSD of Cygnus X-1 : Break BH Mass vs. Break Time Scale Uttley et al. 2004, MNRAS

  10. 3C 120 X-Ray Power Spectral Density (PSD) Break Frequency =10-5 Hz Break Time Scale =2 Days

  11. 3C 120 BH Mass vs. Break Time Scale X-Ray PSD of Cygnus X-1 : Break Uttley et al. 2004, MNRAS, 348, 783

  12. 3C 111 3C 120 BH Mass vs. Break Time Scale X-Ray PSD of Cygnus X-1 : Break These radio galaxies have characteristic timescales similar to the Galactic BH systems =>Accretion processes in a large range of BH masses (10-108 Msun) have similar properties Uttley et al. 2004, MNRAS, 348, 783

  13. Superluminal Ejections Follow X-ray Dips in 3C 111 • X-rays are produced in the accretion disk, radio emission is from the jet • Connection between X-ray and radio emission => Connection between accretion disk and jet Chatterjee et al. 2009, in preparation

  14. Superluminal Ejections Follow X-ray Dips in 3C 120 Chatterjee et al. 2009, ApJ, in press

  15. OUTLINE • 3C 120, 3C 111: Characteristic timescale • 3C 120, 3C 111: Accretion disk-jet connection

  16. Possible Explanation of theX-ray Dip and Superluminal Ejection Correlation • Change in the magnetic field configuration in the accretion disk from turbulent to aligned • absence of viscous heating causes dips in X-ray production • aligned B field configuration facilitates shock to move toward the jet (Livio et al. 2003) X-ray production Weaker flow in the jet Turbulent Decrease in X-ray production Increase in flow in the jet Aligned

  17. Conclusions • Similar characteristic timescale in accreting BH systems of masses 10-108 Msun • Connection between accretion disk and jet • Similarity with galactic black hole X-Ray Binaries: Universality of BH systems

  18. Time-Variability of Active Galactic Nuclei THE END

  19. 3C 120 X-Ray Power Spectral Density (PSD) Break Frequency =10-5 Hz Break Time Scale =2 Days

  20. X-rays corona UV accretion disk BH The Accretion-Disk/Corona Complex Simple modeling of the above system

  21. AGN : Schematic Model Cartoon courtesy: Prof. Alan Marscher

  22. Superluminal Ejections Follow X-ray Dips in 3C 120 Chatterjee et al. 2009, ApJ, in press

  23. X-ray/37 GHz Anti-correlation (X-ray leads 37GHz by 120 days) Chatterjee et al. 2009, ApJ, in press

  24. Possible Explanation of theX-ray Dip and Superluminal Ejection Correlation • Corona is the base of the jet • decrease in the number density of electrons at the base of the jet • causes decrease in X-ray production • increase in the speed of particles (continuity eqn.) => shock wave.

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