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) X-Ray (RXTE-PCA) and VLBA: A. Marscher, S. Jorstad (BU) 37 GHz : Anne Lahteenmaki, Merja Tornikoski, Talvikki Hovatta (Metsahovi Observatory, Finland). 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) 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). 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 Courtesy: C.M. Urry & P. Padovani Blazar BLRG 3C 120 and 3C 111 are BLRGs

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

7 3C BLRG 2. FR-II 3. z= Angle between jet axis and line of sight ~20 o 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 Uttley et al. 2004, MNRAS, 348, 783 X-Ray PSD of Cygnus X-1 : Break BH Mass vs. Break Time Scale 3C 120

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

13 Superluminal Ejections Follow X-ray Dips in 3C 111 Chatterjee et al. 2009, in preparation 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

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 the X-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) Turbulent X-ray production Weaker flow in the jet Aligned Decrease in X-ray production Increase in flow in the jet

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

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

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

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

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

25 Possible Explanation of the X-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.