Copenhagen, Sep. 10th 2008

Is the ejection of the corona a general phenomenon in

microquasars?

Is the ejection of the corona a general phenomenon in

microquasars?

J. Rodriguez & L. Prat (CEA Saclay, France)

with special thanks to M. Coriat and S. Corbel

J. Rodriguez & L. Prat (CEA Saclay, France)

with special thanks to M. Coriat and S. Corbel

Rencontres de Moriond, La Thuile, Feb. 2009

SummarySummary Microquasars :

Definition(some) Light curvesModel independent view: the Q-shape

Accretion-ejection connections:Historically: GRS 1915+105Some more examples: XTE J1748-288, XTE

J1856+229, Cyg X-1

Beyond the phenomenology: physics of outbursts

First steps with XTE J1550-564 and GRS 1915+105: ejection of the corona

What about other sources: the cases of XTE J1748-288, XTE J1856+229, GX 339-4

Conclusions

Microquasars :Definition(some) Light curvesModel independent view: the Q-shape

Accretion-ejection connections:Historically: GRS 1915+105Some more examples: XTE J1748-288, XTE

J1856+229, Cyg X-1

Beyond the phenomenology: physics of outbursts

First steps with XTE J1550-564 and GRS 1915+105: ejection of the corona

What about other sources: the cases of XTE J1748-288, XTE J1856+229, GX 339-4

Conclusions

Rencontres de Moriond, La Thuile, Feb. 2009

Thermal emission: BB ~1 keV

Thermal emission: BB ~1 keV

Non-thermal emission: inverse Compton or Synchrotron: 10 keV-1 MeV

Non-thermal emission: inverse Compton or Synchrotron: 10 keV-1 MeV

}Timing “Noise”, LF & HF QPO: global movement of disc? Of corona? Other mechanism(s)?

Self-absorbed or not Synchrotron: large -> IR/Visible}

Microquasars and diagnosticsMicroquasars and diagnostics

Rencontres de Moriond, La Thuile, Feb. 2009

Microquasars in outburstMicroquasars in outburst

GRS 1915+105

XTE J1859+226

XTE J1748-288

RXTE/ASM

GBI

GBI

RXTE/ASM

RXTE/ASM

RXTE/ASM

Ryle

Rencontres de Moriond, La Thuile, Feb. 2009

A model-independent viewA model-independent view

Fender et al. ‘05; Homan & Belloni ‘05; Remillard & Mc Clintock ‘06

Rencontres de Moriond, La Thuile, Feb. 2009

Accretion-ejection connectionsAccretion-ejection connections

Mirabel et al. ‘98

Rodriguez et al. ‘08

RXTE+IR+Radio => 1st direct link between accretion and ejection (Mirabel et al. ‘98)

INTEGRAL+Ryle => generalisation of this phenomenon: Ejection always follows sequence of spectrally hard dip ended by sudden spike (R. et al. ‘08)

RXTE+IR+Radio => 1st direct link between accretion and ejection (Mirabel et al. ‘98)

INTEGRAL+Ryle => generalisation of this phenomenon: Ejection always follows sequence of spectrally hard dip ended by sudden spike (R. et al. ‘08)

Rencontres de Moriond, La Thuile, Feb. 2009

Towards a general picture?Towards a general picture? GX 339-2

XTE J1859+226 XTE J1748-288

Cyg X-1

Wilms et al. ‘07

Courtesy M. Coriat

Rencontres de Moriond, La Thuile, Feb. 2009

Beyond the phenomenology: ejection of coronal material?

Beyond the phenomenology: ejection of coronal material?

Fits to X-ray data:Behaviour and flux of various spectral components during outbursts

Rodriguez et al. ‘03

XTE J1550-564

Radio detection with ATCA (Corbel et al. ‘01)

Rencontres de Moriond, La Thuile, Feb. 2009

GRS 1915+105GRS 1915+105

I IVII III

Approach of disc + Compton component shrinks between II and III (R. et al. ‘08)

Rencontres de Moriond, La Thuile, Feb. 2009

XTE J1748-288XTE J1748-288

disc flux coronal flux

More complex morphology of radio outburst: multiple flares

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XTE J1859+226XTE J1859+226

Evolution of fluxes not conclusive

Evolution of fluxes not conclusive

However:ykTe max(, 2) With max(, 2)R, mean number of scattering factor 10

Rencontres de Moriond, La Thuile, Feb. 2009

GX 339-4GX 339-4

Compton flux before radio flare

Y shrinks before radio flare => decrease of coronal density

Disc remains ~stable

Compton flux before radio flare

Y shrinks before radio flare => decrease of coronal density

Disc remains ~stable

Soft Soft StateStateSoft Soft

StateState

Hard Hard StateStateHard Hard StateState

Compton Compton fluxflux

Compton Compton fluxflux

yyyy

Radio FlareRadio FlareRadio FlareRadio Flare

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ConclusionsConclusions

Evolution of fluxes: Ejection of the corona pretty clear in 3 sources (1550-564, 1915+105, GX339-4): coronal flux shrinks before the ejection

Fluxes not conclusive in 1748-288 and 1859+226

Physical properties of corona: in 1915+105, 1748-288, 1859+226, and GX 339-4: Comptonisation still in action after ejection, but physical properties of the corona drastically change: xR shrinks <=> (partial) ejection of coronal material

Evolution of fluxes: Ejection of the corona pretty clear in 3 sources (1550-564, 1915+105, GX339-4): coronal flux shrinks before the ejection

Fluxes not conclusive in 1748-288 and 1859+226

Physical properties of corona: in 1915+105, 1748-288, 1859+226, and GX 339-4: Comptonisation still in action after ejection, but physical properties of the corona drastically change: xR shrinks <=> (partial) ejection of coronal material

Rencontres de Moriond, La Thuile, Feb. 2009

The futureThe future Several other candidates: H1743-322/IGR J17464-3213 4U 1543-47 XTE J1908+094 GRO J1655-40 Cyg X-1 ? Cyg X-3 ? Aql X-1 ?

Several other candidates: H1743-322/IGR J17464-3213 4U 1543-47 XTE J1908+094 GRO J1655-40 Cyg X-1 ? Cyg X-3 ? Aql X-1 ?

H1743-322

4U 1543-47

XTE J1908+094