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