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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. Summary. Microquasars : Definition (some) Light curves Model independent view: the Q-shape Accretion-ejection connections:

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Is the ejection of the corona a general phenomenon in microquasars?

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  1. 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

  2. Summary • Microquasars : • Definition • (some) Light curves • Model independent view: the Q-shape • Accretion-ejection connections: • Historically: GRS 1915+105 • Some 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

  3. Microquasars and diagnostics } Self-absorbed or not Synchrotron: large  -> IR/Visible Thermal emission: BB ~1 keV } Timing “Noise”, LF & HF QPO: global movement of disc? Of corona? Other mechanism(s)? Non-thermal emission: inverse Compton or Synchrotron: 10 keV-1 MeV

  4. Microquasars in outburst XTE J1859+226 GBI RXTE/ASM RXTE/ASM GRS 1915+105 RXTE/ASM XTE J1748-288 GBI Ryle RXTE/ASM

  5. A model-independent view Fender et al. ‘05; Homan & Belloni ‘05; Remillard & Mc Clintock ‘06

  6. Accretion-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)

  7. Towards a general picture? GX 339-2 Cyg X-1 XTE J1859+226 XTE J1748-288 Wilms et al. ‘07 Courtesy M. Coriat

  8. Beyond the phenomenology: ejection of coronal material? XTE J1550-564 Rodriguez et al. ‘03 Fits to X-ray data: • Behaviour and flux of various spectral components during outbursts Radio detection with ATCA (Corbel et al. ‘01)

  9. GRS 1915+105 I II III IV Approach of disc + Compton component shrinks between II and III (R. et al. ‘08)

  10. XTE J1748-288 disc flux coronal flux More complex morphology of radio outburst: multiple flares

  11. XTE J1859+226 Evolution of fluxes not conclusive However: ykTe max(, 2) With max(, 2)R, mean number of scattering  factor 10

  12. GX 339-4 Radio Flare Hard State • Compton flux  before radio flare • Y shrinks before radio flare => decrease of coronal density • Disc remains ~stable Soft State Compton flux y

  13. Conclusions • 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

  14. The future 4U 1543-47 XTE J1908+094 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

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