Astronomy and Astrophysics – Astrophysics
Scientific paper
2007-05-09
Adv.Space Res.42:517-522,2008
Astronomy and Astrophysics
Astrophysics
14 pages, accepted for publication on Advances in Space Research. Based on work presented at the 2006 Cospar Scientific Assemb
Scientific paper
10.1016/j.asr.2007.03.099
In the absence of direct kinematic measurements, the mass of an accreting black hole is sometimes inferred from the X-ray spectral parameters of its accretion disk; specifically, from the temperature and normalization of a disk-blackbody model fit. Suitable corrections have to be introduced when the accretion rate approaches or exceeds the Eddington limit. We summarize phenomenological models that can explain the very high state, with apparently higher disk temperatures and lower inner-disk radii. Conversely, ultraluminous X-ray sources often contain cooler disks with large characteristic radii. We introduce another phenomenological model for this accretion state. We argue that a standard disk dominates the radiative output for radii larger than a characteristic transition radius R_c ~ mdot x R_{ISCO}, where mdot is the accretion rate in Eddington units and R_{ISCO} is the innermost stable orbit. For R_{ISCO} < R < R_c, most of the accretion power is released via non-thermal processes. We predict the location of such sources in a luminosity-temperature plot. We conclude that black holes with masses ~ 50-100 Msun accreting at mdot ~ 10-20 may explain the X-ray properties of many ULXs.
Kuncic Zdenka
Soria Rob
No associations
LandOfFree
Black hole mass estimates from soft X-ray spectra does not yet have a rating. At this time, there are no reviews or comments for this scientific paper.
If you have personal experience with Black hole mass estimates from soft X-ray spectra, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and Black hole mass estimates from soft X-ray spectra will most certainly appreciate the feedback.
Profile ID: LFWR-SCP-O-600245