Slim Disk Model for Ultra-Luminous X-Ray Sources

Abstract

The Ultra Luminous X-ray Sources (ULXs) are unique in exhibiting moderately bright X-ray luminosities, $L_{\rm x} \sim 10^{38-40} {\rm erg~s^{-1}}$, and relatively high blackbody temperatures, $\Tin \sim 1.0-2.0 {\rm keV}$. From the constraint that $L_{\rm x}$ cannot exceed the Eddington luminosity, $L_{\rm E}$, we require relatively high black-hole masses, $M\sim 10-100 M_\odot$, however, for such large masses the standard disk theory predicts lower blackbody temperatures, $\Tin < 1.0$ keV. To understand a cause of this puzzling fact, we carefully calculate the accretion flow structure shining at $\sim L_{\rm E}$, fully taking into account the advective energy transport in the optically thick regime and the transonic nature of the flow. Our calculations show that at high accretion rate ($\dot M \ga 30~L_{\rm E}/c^2$) an apparently compact region with a size of $\Rin \simeq (1-3)\rg$ (with $\rg$ being Schwarzschild radius) is shining with a blackbody temperature of $\Tin \simeq 1.8 (M/10M_\odot)^{-1/4}$ keV even for the case of a non-rotating black hole. Further, $\Rin$ decreases as $\dot M$ increases, on the contrary to the canonical belief that the inner edge of the disk is fixed at the radius of the marginally stable last circular orbit. Accordingly, the loci of a constant black-hole mass on the "H-R diagram" (representing the relation between $L_{\rm x}$ and $\Tin$ both on the logarithmic scales) are not straight but bent towards the lower $M$ direction in the frame of the standard-disk relation.