Galactic Black-Hole Candidates Shining at the Eddington Luminosity

Details Galactic Black-Hole Candidates Shining at the Eddington Luminosity Galactic Black-Hole Candidates Shining at the Eddington Luminosity

Feb 2000

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2000pasj...52..133w&link_type=abstract

Publications of the Astronomical Society of Japan, v.52, p.133.

Astronomy and Astrophysics

Astronomy

123

Accretion, Accretion Disks, Black Holes, Stars: X-Rays

Scientific paper

We discuss distinctive features of luminous accretion disks shining at the Eddington luminosity in the context of galactic black-hole candidates (GBCs). We first note that the standard-disk picture is not applicable, although it is often postulated. Rather, the disk becomes advection-dominated while remaining optically thick (the so-called slim disk). The slim disk exhibits several noteworthy signatures: (1) The disk luminosity is insensitive to the mass-flow rates, dot M, and is always kept around the Eddington luminosity, L_E, even if dot M greatly exceeds L_E/c2. This reflects the fact that radiative cooling is no longer balanced by viscous heating and excess energy is carried by accreting matter to black holes. (2) The spectra of the slim disks are multi-color blackbody characterized by (i) a high maximum temperature, kT_in ~ a few keV, (ii) a small size of an emitting region, r_in < 3 r_g (with r_g being Schwarzschild radius), due to substantial radiation coming out from inside 3 r_g, and (iii) flatter spectra in the soft-X bands, nu S_nu ~ nu 0, because of a flatter effective temperature profile of the slim disk, T_eff~ r-1/2 (in contrast with T_eff~ r-3/4 in the standard disk). Thus, a small r_in (<< 3r_g) does not necessarily mean the presence of a Kerr hole. Furthermore, (3) as dot M increases, T_in increases, while r_in decreases as r_in ~ (T_in)-1 approximately. That is, the changes in r_in derived from the fitting do not necessarily mean the changes in the physical boundary of the optically thick portions of the disk. Observational implications are discussed in relation to binary jet sources.

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