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Radio Observations
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ACCRETION–JET CONNECTION
•THE TRIGGERS OF JETS ARE INSTABILITIES IN THE ACCRETION DISK (TRANSITION LOW HARD TO HIGH THE X-RAY “SPIKE” MARKS THE ONSET OF A SHOCK THROUGH THE COMPACT, STEADY JET •ANALOGOUS ACCRETION-JET CONNECTION IN 3C 120 Marscher (2002)
∆τ α MBHMirabel et al. 1998 1 hr in GRS 1915+105 = 30 yr in SgrA*
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Y
MERLIN 150 Km
VLA 27 KmVLBA
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COMPACT STEADY JETS
• ~100 AU IN LENGTH PRESENT DURING LOW HARD STATE
• SPEED OF THE FLOW < 0.4c (Dhawan, Ribo & Mirabel 2006)
GRS 1915+105: Dhawan, Ribo & Mirabel (2006)
2.0 cm 3.6 cm
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SUPERLUMINAL MOTION IN THE GALAXY
-RELATIVISTIC ABERRATION FROM TWIN JETS SEEN TWO-SIDED
- µQSO JETS MOVE ON THE SKY ~103 TIMES FASTER THAN QSO JETS
- IN AGN AT D<100 Mpc JETS ARE RESOLVED AT ~50 Rsh (e.g. M87,Biretta)
PHYSICS: NEED TO STUDY BHs ACROSS ALL MASS SCALES
Mirabel & Rodriguez, 1994
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Superluminal MotionIndividual radio knots in quasar jets:
Sometimes apparently moving faster than speed of light!
Light-travel time effect:
Material in the jet is almost catching up
with the light it emits
0
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SUPERLUMINAL MOTIONS IN QSOs & AGN
•OBSERVED IN > 30 QSOs & AGN
•IN RADIO & OPTICAL WAVES
• PROPER MOTION SEEN IN YEARS
•Vapp UP TO 30c in blazars
•One sided because of Doppler boosting
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E = γ me c2 γ = 1
1− v2
c2
Electron energy distribution is a power law:
γ>>1
Relativistic electrons in a magnetic field
N E dE=kE p dE
P υ , θ ∝ B p1/2 υ− p−1/2 ∫υ /υ1
υ /υ2
. . . . . . . .α
The radio spectrum is therefore a power law:
S ∝ υ−α α = − p− 1 /2
Typical α~0.8 p~2.6
For one electron, max frequency ¿ γ 2
for slightly different γ covers the entire spectrum
Assuming the emission from each can be added up (optically thin case)
-
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dECEdEEN p−=)(
In this case, we have
21
)(−−
∝p
S νν
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Flux density vs frequency
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Longair
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Flux density (Jy)
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“steep“Optically thin spectra Flat spectra
Fender 2001
STEADY JETSTRANSIENT JETS
Mirabel .& Rodrigez 1994
Fender et al. 2001, 2004,2006
Dhawan et al. 2000
Steady Jets and Transient Jets- Bonn 2010 M. Massi
GRS 1915+105GRS 1915+105
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The radio-optical spectrum of XRBs
• Radio-to-NIR spectrum is flat in the hard state.
(Fender 2000)
V404 Cyg
www.astro.isas.ac.jp/conference/bh2003/program/ppt/20031029am/KyotoBH2003_Falcke.ppt
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ν
Sν
RADIO SPECTRUM: WHY IS IT “FLAT” ?
νb r e a k
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Dulk (1985), Ann. Rev. Astronomy & Astrophysics, 23, 183
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Mbh~10
Sν
JET
Blandford & Konigl 1979; Hjellming & Johnston 1988; Falcke et al. 1996; Kaiser 2006; Pe'er &Casella 2009)
Change of the plasma conditions along the jet:
decay of the magnetic field
change in the electron energy distribution
νb r e a k
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ν
Mbh~10
Sν
JET1
1
Blandford & Konigl 1979; Hjellming & Johnston 1988; Falcke et al. 1996; Kaiser 2006; Pe'er &Casella 2009
1
dependence of the “break” frequency on the changing plasma conditions
along the jet
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ν turnover frequency in stellar black holes > blazars ( BXRB>>BAGN)
Sν
Mbh~109Rmin
ν max~1013 Hz
Sν ~ ν-0.7
Radio/mm
ν
Sν
Mbh~10Rmin
ν max~1015 Hz
Opt/UV/XRadio/mm
www.astro.isas.ac.jp/conference/bh2003/program/ppt/20031029am/KyotoBH2003_Falcke.ppt
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Steady Radio JetSteady Radio Jet slow velocity slow velocity ~0.1 c
Continuousconical jet centered on the centered on the systemsystem, flat radio spectrum
Dhawan et al. 2000
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GRS 1915+105
Dhawan et al 2000
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Two distinct radio emission states
radio emission attached to..................... and detached from the center
Mirabel .& Rodrigez 1994
GRS 1915+105
GRS 1915+105
Dhawan et al. 2000
GRS 1915+105
GRS 1915+105
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X-ray State
Low Hard
“steep“Optically thin spectra Flat spectra
Fender 2001
X-ray State
Steep Power-low State
STEADY JETSTRANSIENT JETS
Mirabel .& Rodrigez 1994
Steady Jets and Transient Jets- Bonn 2010 M. Massi
Dhawan et al. 2000
Fender et al. 2001
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Accretion states
Photon cm-2 s-1 keV-1
1 10 100 1 10 100 1 10 100Energy (keV)
Energy spectra from McClintock & Remillard (2006)
High
(thermal dominated)~ 1 – 2 keV disc + PL tail
Very High
(steep power-law)Soft PL (Γ > 2.5) plus some hot disc emission. Most luminous.
Low/HardHard PL (Γ ~ 1.5 – 2)
dominant, disc absent or truncated, radio jet
emission. Least luminous.
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Hard SPL Thermal
Distributions in Photon Index
Ron RemillardRon Remillard
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Radio/X-ray Flux Correlation
Corbel et al. (2000,2003)Fradio ∝ FX+0.7
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Radio/X-ray Flux Correlation
Corbel et al. (2000,2003)Fradio ∝ FX+0.7
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www.astro.lsa.umich.edu/Events/Meetings/mctpwww/.../Fender.ppt
X-ray hardness
X-ray Lum
inosity / Eddington
<10-6
~0.01
~0.1
~1.0
softspectrum
hardspectrum
Hardness ratio: the ratio of detector counts in two energy bands
( example. the ratio of source counts at 6.3–10.5 keV to the counts at 3.8–7.3 keV)
Transient
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Powerful jets produced in transition from canonical ‘low/hard’ to ‘high/soft’ states…
Fender, Belloni & Gallo (2004)
Gallo et al. 2004
Homan & Belloni 2005
Gallo et al. 2004
http://www.astro.lsa.umich.edu/Events/Meetings/mctpwww/contrib.htmlFender.ppt
GX339-4
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Black Hole States: Statistics
Timescales (days) for state (all BH Binaries) duration transitions
Steep Power Law 1-10 <1
Low/hard 3-200 1-5
Ronald Remillard
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STEADY
JET
TRANSIENT
JETIn analogy with solar flares, magnetic energy is probably built-up and accumulated over long time scales and then dissipated in very short time
On the other hand the removal of angular momentum via the steady jet has a dramatic effecton the overall process of the accretion process, further increasing the twist of the magnetic field and making magnetic reconnection among tangled field lines likely to occur.
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Marscher & Gear shock-in-jet model (1985) Gallo et al. 2004
New highly-relativistic plasma catches up the pre-existing slower-moving material of the steady jet steady jet giving rise to shocks...
..that produce the optically thin outburst.
http://isdc.unige.ch/~turler/jets/
Marc Türler Marc Türler's review
Gallo et al. 2004