Copenhagen, Sep. 10 th 2008 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 Summary G Microquasars : G Definition G (some) Light curves G Model independent view: the Q-shape G Accretion-ejection connections: G Historically: GRS G Some more examples: XTE J , XTE J , Cyg X-1 G Beyond the phenomenology: physics of outbursts G First steps with XTE J and GRS : ejection of the corona G What about other sources: the cases of XTE J , XTE J , GX G Conclusions G Microquasars : G Definition G (some) Light curves G Model independent view: the Q-shape G Accretion-ejection connections: G Historically: GRS G Some more examples: XTE J , XTE J , Cyg X-1 G Beyond the phenomenology: physics of outbursts G First steps with XTE J and GRS : ejection of the corona G What about other sources: the cases of XTE J , XTE J , GX G Conclusions

Rencontres de Moriond, La Thuile, Feb Thermal emission: BB ~1 keV 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 diagnostics

Rencontres de Moriond, La Thuile, Feb Microquasars in outburst GRS XTE J XTE J RXTE/ASM GBI RXTE/ASM Ryle

Rencontres de Moriond, La Thuile, Feb A model-independent view Fender et al. 05; Homan & Belloni 05; Remillard & Mc Clintock 06

Rencontres de Moriond, La Thuile, Feb Accretion-ejection connections Mirabel et al. 98 Rodriguez et al. 08 G RXTE+IR+Radio => 1st direct link between accretion and ejection (Mirabel et al. 98) G INTEGRAL+Ryle => generalisation of this phenomenon: Ejection always follows sequence of spectrally hard dip ended by sudden spike (R. et al. 08) G RXTE+IR+Radio => 1st direct link between accretion and ejection (Mirabel et al. 98) G 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 Towards a general picture? GX XTE J XTE J Cyg X-1 Wilms et al. 07 Courtesy M. Coriat

Rencontres de Moriond, La Thuile, Feb 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 J Radio detection with ATCA (Corbel et al. 01)

Rencontres de Moriond, La Thuile, Feb GRS I IV II III Approach of disc + Compton component shrinks between II and III (R. et al. 08)

Rencontres de Moriond, La Thuile, Feb XTE J disc fluxcoronal flux More complex morphology of radio outburst: multiple flares

Rencontres de Moriond, La Thuile, Feb XTE J Evolution of fluxes not conclusive However: y kT e max(, 2 ) With max(, 2 ) R, mean number of scattering factor 10

Rencontres de Moriond, La Thuile, Feb GX G Compton flux before radio flare G Y shrinks before radio flare => decrease of coronal density G Disc remains ~stable Soft State Hard State Compton flux yy Radio Flare

Rencontres de Moriond, La Thuile, Feb Conclusions G Evolution of fluxes: Ejection of the corona pretty clear in 3 sources ( , , GX339-4): coronal flux shrinks before the ejection G Fluxes not conclusive in and Physical properties of corona: in , , , 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 The future Several other candidates: G H /IGR J G 4U G XTE J G GRO J G Cyg X-1 ? G Cyg X-3 ? G Aql X-1 ? H U XTE J