observational overview of state transitions in x-ray binaries

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JETS radio and nIR monitoring: lots of progress We can try to do the same for jets. How does jet activity map onto the HID? The last decade has seen an enormous increase in the amount of radio and near-infrared observations, both of which can be used to study the evolution of jet outflows.
No Compact Jet (interaction with ISM) Fender, Belloni, Gallo 2004 Fender, Homan, Belloni, 2009 soft Ejection Events rms-drop type-B QPOs JETS Compact Jet Switches on (radio) Radio Flare hard Compact Jet Weakens (radio/nIR) Compact Jet Compact Jet Switches on (nIR) Homan et al. 2005 Russell et al. 2006 Coriat et al. 2009 I’m going to use the same schematic again and will summarize the picture that is emerging from various radio and nIR papers. I’ll start with the hard state and progress through the diagram in an anti-clockwise manner. The hard state gives rise to steady radio emission from a compact jet. Radio and nIR emission scale in similar ways with the X-ray luminosity. Once a system turns the corner the radio and nIR start to weaken, suggesting the jet is getting less powerful. Than at some point during the transition a radio flare is observed, which is thought to be the result of an ejection event. Interestingly, this flare always seems to take place within a few days of this zone with odd variability properties that I just discussed. In sources that cross this zone multple times during an outburst, like XTE J1858+226, we see radio flares associated with rms drops in all cases. Bright sources that enter the steep power law state suggest that ejection events continue to occur in that state. No radio emission from the central source is seen in the soft state. If there is radio emission it is likely the result of interaction of the jet ejecta with the ISM. At some point the source starts it return to the hard state. We’re not exactly sure when the jet switches on again in the radio, but from at least one source it is clear that it start somewhere halfway in the transition, and perhaps even earlier. In the near-infrared jet emission only becomes significant when it reaches the hard state.
Page 1 and 2: !""#$%&'()*#'"$++$+)&(),-#!.+/ 4566
Page 3 and 4: MORE BACKGROUND • 1996>: Dedicate
Page 5 and 6: TRANSIENT SOURCES • Relation betw
Page 7 and 8: OUTBURST LIGHT CURVES 4U 1543-47 GR
Page 9 and 10: ENERGY DEPENDENCE This movie (Homan
Page 11 and 12: SPECTRAL EVOLUTION GX 339-4 First I
Page 13 and 14: COLOR EVOLUTION hardness-intensity
Page 15 and 16: Luminosity (erg/s) SPECTRAL EVOLUTI
Page 17 and 18: XTE J1752-223 XTE J1908+094 SPECTRA
Page 19 and 20: SPECTRAL EVOLUTION GRO J1655-40 I
Page 21 and 22: SPECTRAL EVOLUTION GRO J1655-40 We
Page 23 and 24: SPECTRAL EVOLUTION GX 339-4 Transit
Page 25 and 26: IMPLICATIONS FOR ACCRETION • outb
Page 27 and 28: STATE CLASSIFICATION • Various cl
Page 29 and 30: RAPID X-RAY VARIABILITY • power d
Page 31 and 32: • low-luminosity version of the h
Page 33 and 34: INTERMEDIATE STATE Intermediate (tr
Page 35 and 36: RAPID X-RAY VARIABILITY Okay, let
Page 37: Power type-B frequency up 1 10 100
Page 41 and 42: GRO J1655-40 weak abs. lines weak e
Page 43 and 44: Aql X-1 NEUTRON STARS hard - soft -
Page 45 and 46: Aql X-1 Back to the HID again. NEUT
Page 47 and 48: hard transitional Lin et al. 2009 H
Page 49 and 50: Lin et al. 2009 Homan et al. 2010 N

observational overview of state transitions in x-ray binaries

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