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X-rays from Quiescent Black Holes: Accretion or Jet Powered?

X-rays from Quiescent Black Holes: Accretion or Jet Powered?. Wei Cui Purdue University. Collaborators: Gabor Pszota, Purdue University Feng Yuan, Shanghai Astronomical Observatory Hui Zhang, Shanghai Astronomical Observatory. Stellar-Mass Black Holes.

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X-rays from Quiescent Black Holes: Accretion or Jet Powered?

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  1. X-rays from Quiescent Black Holes: Accretion or Jet Powered? • Wei Cui • Purdue University • Collaborators: • Gabor Pszota, Purdue University • Feng Yuan, Shanghai Astronomical Observatory • Hui Zhang, Shanghai Astronomical Observatory

  2. Stellar-Mass Black Holes • 21 dynamically determined BH X-ray binaries • about 2 dozens more BH candidates • Only 4 are persistent X-ray sources • all with OB secondary stars • Transients constitute the majority • nearly all with late-type secondary stars

  3. Outbursts

  4. Spectral States XTE J1550-564 Xue, Wu, & Cui 2008

  5. Low-Hard State Yuan, Cui, & Narayn 2005

  6. Modeling Low-Hard State Yuan, Cui, & Narayn 2005

  7. Extrapolation to Quiescence Yuan & Cui 2005 The shape of X-ray spectra deviates from a power law in the quiescent state.

  8. XMM-Newton Observations • GRO J1655-40: 185 ks, Fx = 5.8 x 10-14 erg s-1 cm-2 • in two segments, separated by about 1 month • XTE J1550-40: 59 ks, Fx = 4.9 x 10-14 erg s-1 cm-2 • but severely contaminated • V404 Cyg: 40 ks, Fx = 40 x 10-14 erg s-1 cm-2 • archival observation

  9. Quiescent X-ray Spectra Pszota et al. 2008

  10. Can AFAF Fit? Pszota et al. 2008

  11. Conclusions • The observed X-ray spectra of GRO J1655-60 and V404 Cyg in the quiescent state deviate strongly from the expectation of ADAF models. • The power-law shape of the X-ray spectra can be explained by a dominant jet contribution. • The case of XTE J1550-564 is still ambiguous, as limited by the statistics of the data. Pszota et al. 2008, MNRAS

  12. Another Test Yuan & Cui 2005

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