Disk-Jet Connection in the Radio Galaxies 3C 120 and 3C 111
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1 Disk-Jet Connection Disk-Jet Connection in the Radio in the Radio Galaxies 3C 120 and Galaxies 3C 120 and 3C 111 3C 111 Ritaban Chatterjee Ritaban Chatterjee NERQUAM 2010, May 18th, 2010. NERQUAM 2010, May 18th, 2010.
description
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). - PowerPoint PPT Presentation
Transcript of Disk-Jet Connection in the Radio Galaxies 3C 120 and 3C 111
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Disk-Jet Connection Disk-Jet Connection in the Radio in the Radio
Galaxies 3C 120 and Galaxies 3C 120 and 3C 1113C 111
Ritaban ChatterjeeRitaban Chatterjee
NERQUAM 2010, May 18th, 2010.NERQUAM 2010, May 18th, 2010.
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Data SourcesData Sources X-Ray (RXTE-PCA) and VLBA: X-Ray (RXTE-PCA) and VLBA: A. Marscher, S. A. Marscher, S.
JorstadJorstad (BU)(BU) 37 GHz : 37 GHz : Anne Lahteenmaki, Merja Anne Lahteenmaki, Merja
Tornikoski, Talvikki HovattaTornikoski, Talvikki Hovatta (Metsahovi (Metsahovi Observatory, Finland).Observatory, Finland).
R Band: R Band: I. McHardyI. McHardy (U. Southampton), (U. Southampton), Kevin Kevin Marshall, H. Richard Miller, Wesley T. RyleMarshall, H. Richard Miller, Wesley T. Ryle (Georgia State)(Georgia State)
V Band: V Band: Large international team (please see Large international team (please see ApJ paper for details) led by Martin GaskellApJ paper for details) led by Martin Gaskell (U. Texas, Austin, U. Nebraska, Lincoln).(U. Texas, Austin, U. Nebraska, Lincoln).
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AGN : Unified Picture
Courtesy: C.M. Urry & P. Padovani
BlazarBLRG 3C 120 and 3C 111
are BLRGs
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Mirabel &Rodriguez 1998,Nature, 392, 673.
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OUTLINE
• 3C 120, 3C 111: Characteristic timescale
• 3C 120, 3C 111: Accretion disk-jet connection
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3C 120
1. BLRG2. FR-I3. z=0.033 4. Angle between jet axis and
line of sight ~20o
5 GHz Image: Walker, Benson & Unwin 1987 ApJ, 316, 546
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3C 1111. BLRG2. FR-II3. z=0.048 4. Angle between jet axis and
line of sight ~20o
1.4 GHz Image: Linfield & Perley 1984, ApJ, 279, 60
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Variability atdifferent timescales
Power Spectral Density (PSD) => Amplitude of variability as a function of timescale
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X-Ray PSD of Cygnus X-1 : Break
BH Mass vs. Break Time Scale
Uttley et al. 2004, MNRAS
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3C 120 X-Ray Power Spectral Density (PSD)
Break Frequency=10-5 HzBreakTime Scale=2 Days
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Uttley et al. 2004, MNRAS, 348, 783
X-Ray PSD of Cygnus X-1 : Break
BH Mass vs. Break Time Scale
3C 120
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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 alarge range of BH masses (10-108 Msun) have similar properties
Uttley et al. 2004, MNRAS, 348, 783
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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
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Superluminal Ejections Follow
X-ray Dips in 3C 120
Chatterjee et al. 2009, ApJ,in press
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OUTLINE
• 3C 120, 3C 111: Characteristic timescale
• 3C 120, 3C 111: Accretion disk-jet connection
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Possible Explanation of thePossible Explanation of the X-ray Dip and X-ray Dip and Superluminal Ejection CorrelationSuperluminal Ejection Correlation
Change in the magnetic field configuration in Change in the magnetic field configuration in the accretion disk from turbulent to aligned the accretion disk from turbulent to aligned
absence of viscous heating causes dips in X-absence of viscous heating causes dips in X-ray production ray production
aligned B field configuration facilitates shock to aligned B field configuration facilitates shock to move toward the jet (Livio et al. 2003)move toward the jet (Livio et al. 2003)
TurbulentX-ray productionWeaker flow in the jet
AlignedDecrease in X-ray productionIncrease in flow in the jet
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ConclusionsConclusions Similar characteristic timescale Similar characteristic timescale
in accreting BH systems of in accreting BH systems of masses masses 10-1010-1088 M Msunsun
Connection between accretion Connection between accretion disk and jetdisk and jet
Similarity with galactic black Similarity with galactic black hole X-Ray Binaries: Universality hole X-Ray Binaries: Universality of BH systemsof BH systems
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Time-Variability of Active Galactic Nuclei
THE END
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3C 120 X-Ray Power Spectral 3C 120 X-Ray Power Spectral Density (PSD)Density (PSD)
Break Frequency=10-5 HzBreakTime Scale=2 Days
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corona
accretion disk BH
X-rays
UV
The Accretion-Disk/Corona The Accretion-Disk/Corona ComplexComplex
Simple modeling of the above system
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AGN : Schematic Model
Cartoon courtesy:
Prof. Alan Marscher
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Superluminal Ejections Follow X-ray Dips in 3C 120
Chatterjee et al. 2009, ApJ,in press
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X-ray/37 GHz Anti-correlation (X-ray leads 37GHz by 120 days)
Chatterjee et al. 2009, ApJ,in press
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Possible Explanation of thePossible Explanation of the X-ray Dip and X-ray Dip and Superluminal Ejection CorrelationSuperluminal Ejection Correlation
Corona is the base of the jet Corona is the base of the jet decrease in the number density of decrease in the number density of
electrons at the base of the jet electrons at the base of the jet causes decrease in X-ray production causes decrease in X-ray production increase in the speed of particles increase in the speed of particles
(continuity eqn.) => shock wave.(continuity eqn.) => shock wave.
