Copenhagen, Sep. 10 th 2008 Is the ejection of the corona a general phenomenon in microquasars? J....

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

Rencontres de Moriond, La Thuile, Feb. 2009

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

Rencontres de Moriond, La Thuile, Feb. 2009

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