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multi-wavelength variability from jets in X-ray binaries - - PowerPoint PPT Presentation

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Beyond X-ray timing II: variability from jets P. Casella - Soton BH Variability /34 1 Beyond X-ray timing II: multi-wavelength variability from jets in X-ray binaries Piergiorgio Casella (University of Southampton) Beyond X-ray timing II:

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Beyond X-ray timing II:

multi-wavelength variability from jets in X-ray binaries

Piergiorgio Casella

(University of Southampton)

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  • utline

why jets why jets variability jets variability!

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why are jets important?

AGN - X-ray Binaries - GRBs - WDs - SNe - Protostars - (ULX?) General phenomenon >>> general knowledge

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AGN XB SN remnant protostar

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why are jets important?

AGN - X-ray Binaries - GRBs - WDs - SNe - Protostars - (ULX?) General phenomenon >>> general knowledge They influence the evolution of the launching system They influence their surroundings (ISM, IGM) Jet launching mechanisms are unknown Jet structure and composition are often unknown They can be launched from, or close to, a strong-gravity environment Jets in XBs vary on timescales from years to milliseconds

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Jet companion star high energy tail (inner regions)

X-ray IR opt radio

BH

hard state

Disc

multi-wavelength spectrum

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companion star

X-ray IR opt radio

BH

soft state

Jet high energy tail (inner regions) Disc

multi-wavelength spectrum

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/34 8 Fender, Belloni & Gallo 2004

jet evolution: coupling with X-rays

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/34 9 Gallo et al. 2003 ; Soleri et al. 2010

Swift J1753.5-0127 Swift J1753.5-0127 3 upper limits

1E1740.7-2942 4U 1543-47 A0620-00 GRO J0422+32 GRS 1758-258 GS 1354-64 GX 339-4 GX 339-4, 3 upper limits IGR J17497-2821, 3 upper limits XTE J1118+480 XTE J1550-564 XTE J1550-564, 3 upper limits XTE J1650-500 XTE J1720-318, 3 upper limits XTE J1720-318 V404 Cyg Swift J1753.5-0127 detections 3 upper limits

Outliers, from Gallo (2007): Data used in Gallo et al. (2006):

H 1743-322, from Jonker et al. (2010) and McClintock et al. (2009): bG06~0.58 b~1.0 b~1.4

jet evolution: coupling with X-rays

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The radio-flat jet paradigm

ν

Flux

νobs

Total spectrum results from summed contributions at each distance z along the jet z

synchrotron losses should act very fast.. ...need for extra energy for the electrons!

a problem: the missing re-heating

picture from Markoff 2010

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The radio-flat jet paradigm

ν

Flux

νobs

Total spectrum results from summed contributions at each distance z along the jet z

synchrotron losses should act very fast.. ...need for extra energy for the electrons!

a problem: the missing re-heating

picture from Markoff 2010

Unless B-field is very low:

much lower than equipartition with electron energy. In this case, maybe, you can make it without re-heating...

Pe’er & Casella 2009

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illustration of shells in our jet model. If the outer boundary of the inner shell, (j), contacts the inner boundary of the outer

Jamil, Fender & Kaiser 2010

a possibility: internal shocks between discrete shells with different velocity.

The radio-flat jet paradigm

a problem: the missing re-heating

IS THE JET POWERED BY VARIABILITY FROM THE ACCRETION FLOW?

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illustration of shells in our jet model. If the outer boundary of the inner shell, (j), contacts the inner boundary of the outer

Jamil, Fender & Kaiser 2010

IS THE JET POWERED BY VARIABILITY FROM THE ACCRETION FLOW?

The radio-flat jet paradigm

courtesy of Omar Jamil

!"#$%&%'(%)#!**+ ,-./#01.2%)3.45 !*

!"#$%&'()*+',-.'

!"#$%&#'(')'*$%+,-(.%$/(01%020$%*(','345(#+--'-

67,'345( '8"%&03$%$%+,( 2'$.'',( 904,'$%*:( '#'*$3+,:(0,1( $/'390#(','345 6;<4=(')'*$%+,( 40&(>(?- 6@%9=(1"30$%+,A BC?DE(- 6F,%$%0#(%,$'3,0#( ','345(%,)'*$%+,( !"#"$$%&'

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first there was X-ray emission then the jet

Hesiod 8th-7th century BC

chaos

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/34 15 Mirabel et al. 1998

from X-rays...all the way into the jet

radio follows IR which follows X-rays

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/34 16 Mirabel et al. 1998

from X-rays...all the way into the jet

radio follows IR which follows X-rays

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from X-rays...all the way into the jet

radio follows IR by a 7 (or 33) minutes

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from X-rays...all the way into the jet

clear need for a proper timing analysis either longer observations

  • r higher time resolution

teo’s talk: we can go fast in optical!

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CCFfg(t)=

8 + 8

  • f(τ) g(τ+t) dτ

.

Hynes et al. 2009

Reprocessed variability:

O’Brien et al. 2002

let’s go faster: X-ray/optical CCFs

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X-ray/opt CCF

The optical variability is anti-correlated, and precedes the X-rays! Not reprocessing...what?

Kanbach et al. 2001 ( e.g. Hynes et al. 2003 )

Reprocessed variability:

O’Brien et al. 2002

≠

let’s go faster: X-ray/optical CCFs

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X-ray/opt CCF

The optical variability is anti-correlated, and precedes the X-rays! Not reprocessing...what?

Kanbach et al. 2001 ( e.g. Hynes et al. 2003 )

let’s go faster: X-ray/optical CCFs

Hynes et al. 2003

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The “common reservoir model” (Malzac, Merloni & Fabian 2004) jet-corona coupling through common energy reservoir accretion flow (reservoir)

  • ptical

from the jet X-rays from the corona

an explanation: a powerful jet

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The “common reservoir model” (Malzac, Merloni & Fabian 2004) jet-corona coupling through common energy reservoir if the system is “jet dominated”, it works:

an explanation: a powerful jet

Data Model

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2001: XTE J1118 (a BH) 2008 (other 2 BHs): GX 339-4 SWIFT J1753 too many components?

Kanbach et al. 2001 Gandhi et al. 2008 Durant et al. 2008

reality seems more complex: The “common reservoir model” (Malzac, Merloni & Fabian 2004) jet-corona coupling through common energy reservoir

an explanation: a powerful jet

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let’s go faster: X-ray/optical QPOs (jet?)

Hynes et al. 2003 Gandhi et al. 2009

GX 339-4 XTE J1118+480

0.01 0.1 1 10 Frequency [Hz] 0.001 0.010 0.100 1.000 Power [ (rms/mean)2 Hz-1 ] Optical Optical X-ray X-ray 0.01 0.1 1 10 Frequency [Hz] 0.001 0.010 0.100 1.000 Power [ (rms/mean)2 Hz-1 ] Optical Optical X-ray X-ray 0.01 0.1 1 10 Frequency [Hz] 0.001 0.010 0.100 1.000 Power [ (rms/mean)2 Hz-1 ] Optical Optical X-ray X-ray 0.01 0.1 1 10 Frequency [Hz] 0.001 0.010 Freq x Power [ Hz (rms/mean)2/Hz ] Optical Optical X-ray X-ray 0.01 0.1 1 10 Frequency [Hz] 0.001 0.010 Freq x Power [ Hz (rms/mean)2/Hz ] Optical Optical X-ray X-ray 0.01 0.1 1 10 Frequency [Hz] 0.001 0.010 Freq x Power [ Hz (rms/mean)2/Hz ] Optical Optical X-ray X-ray

BUT: the same QPO COULD be present in X-rays. the only ‘fact’ is that in optical the QPO is relatively stronger

Gandhi et al. (submitted)

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Jet companion star high energy tail (inner regions)

X-ray IR opt radio

BH

hard state

Disc

if you want the jet..go where the jet is

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GX 339-4 - ISAAC@VLT - 62.5ms - K=12.5

23’’ x 23’’

let’s go redder: infrared fast photometry!

So far, in optical. The jet/disk ratio is (much) higher in infrared

X-rays infrared

I S A A C R X T E

Casella, Maccarone et al. 2010

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X-rays infrared

I S A A C R X T E

let’s go redder: infrared fast photometry!

So far, in optical. The jet/disk ratio is (much) higher in infrared

R X T E I S A A C

GX 339-4 - ISAAC@VLT - 62.5ms - K=12.5

Casella, Maccarone et al. 2010

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Jet companion star high energy tail (inner regions)

X-ray IR opt radio

BH

hard state

Disc

let’s go redder: infrared fast photometry!

Russell et al (in prep.)

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let’s go redder: infrared fast photometry!

So far, in optical. The jet/disk ratio is (much) higher in infrared GX 339-4 - ISAAC@VLT - 62.5ms - K=12.5

Infrared and X-rays are correlated Infrared lag X-rays by 0.1 s Very high brightness temperature (>106K) We are observing the JET It takes 0.1s for the matter to get there

Γ > 2 (model dependent)

Casella, Maccarone et al. 2010

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let’s go redder: infrared fast photometry!

So far, in optical. The jet/disk ratio is (much) higher in infrared GX 339-4 - ISAAC@VLT - 62.5ms - K=12.5

  • we assume all jets in X-ray binaries are similar
  • we scale from Cyg X-1 in radio to GX 339-4 in infrared
  • measure the speed for many sets of parameters

rmax ~ γ-4/3 β-2/3 D 2/3 sinθ-1/3 Φ-1 L2/3 ν-1 ( “standard” formula by Blandford & Königl ’79 )

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let’s go redder: infrared fast photometry!

So far, in optical. The jet/disk ratio is (much) higher in infrared GX 339-4 - ISAAC@VLT - 62.5ms - K=12.5

rmax ~ γ-4/3 β-2/3 D 2/3 sinθ-1/3 Φ-1 L2/3 ν-1 ( “standard” formula by Blandford & Königl ’79 )

  • we assume all jets in X-ray binaries are similar
  • we scale from Cyg X-1 in radio to GX 339-4 in infrared
  • measure the speed for many sets of parameters

Γ > 2

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let’s go redder: infrared fast photometry!

So far, in optical. The jet/disk ratio is (much) higher in infrared GX 339-4 - ISAAC@VLT - 62.5ms - K=12.5

  • if we assume: E0 ~ X-ray
  • if we assume: “cooling time” ~ time delay
  • we observe E1 ~ infrared

}

  • γ0 ~ 104
  • γ1 ~ 50
  • B ~ 104 G

We are measuring physical quantities... ...many uncertainties, but this is “day zero”

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This is a relatively new field. There is much to do Jets vary, we just don’t know how yet. We can learn a lot!

  • we OBSERVE matter while it goes along the jet
  • we can MEASURE physical quantities
  • (this ain’t necessarily true of course...)

Jets are ubiquitous: general knowledge: easy to sell! Parallel observational/theoretical/numerical efforts:

  • collecting (fast) data in opt, near-IR, mid-IR, soft/hard X-rays...
  • developing new jet variability models (O. Jamil - A. Pe’er - ...)
  • getting used to timing techniques

Nevertheless, we need new instrumentation

  • simultaneous optical-infrared fast timing (we are doing it! but difficult)
  • fast-photometers permanently mounted, for ToO & monitoring

The future: E-ELT: huge statistics! population statistics

X

will

discussion - conclusions - future