The Hard X-ray Spectral Evolution in XRBs, AGNs and ULXs

Details The Hard X-ray Spectral Evolution in XRBs, AGNs and ULXs The Hard X-ray Spectral Evolution in XRBs, AGNs and ULXs

2008-12-17

arxiv.org/abs/0812.3290v1

Astronomy and Astrophysics

Astrophysics

5 pages, 1 figure, accepted for pulication in Proceeding of SCience, VII Microquasar Workshop, 2008 September 1-5, Foca, Turke

Scientific paper

We explore the relationship between the hard X-ray photon index $\Gamma$ and the Eddington ratio (\xi=L_{X}(0.5-25 keV)/L_{Edd}) in six XRBs. We find that different XRBs follow different anti-correlations between $\Gamma$ and $\xi$ when $\xi$ is less than a critical value, while they follow the same positive correlation when $\xi$ is larger than the critical value. This anti-correlation and positive correlation are also found in LLAGNs and QSOs respectively, and the anti-correlation and positive correlation of different XRBs roughly converge to the same point ($\log \xi=-2.1, \Gamma=1.5$), which may correspond to the accretion mode transition, since that the anti-correlation and positive correlation are consistent with the prediction of ADAFs and standard disk/corona system respectively. The traditional low/hard state are divided into two parts by the cross point $\log \xi\sim-2.1$, i.e., faint-hard state in the anti-correlation part and bright-hard state in the positive correlation part. The accretion process in the bright-hard state may be still the standard accretion disk as that in the high/soft state, which is consistent with that both the cold disk component and broad Fe K emission line are observed in some bright-hard state of XRBs. The ADAF is only important in the faint-hard state XRBs. Motivated by the similarities of the state transition and timing properties of the ULXs to that of XRBs, we then constrain the BH masses for seven luminous ULXs assuming that their X-ray spectral evolution is similar to that of XRBs. We find that the BH masses of these seven ULXs are around $10^{4}M_sun$, which are typical intermediate mass BHs (IMBHs). Our results are roughly consistent with the BH masses constrained from the model fitting with a multi-color disk and/or the timing properties(e.g., QPO and break frequency).

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