R. Sunyaev

Black holes in binary systems. Observational appearance

The outward transfer of angular momentum of accreting matter can lead to the formation of a disk around the black hole. The structure and radiation spectrum of the disk depends, in the main, on the rate of matter inflow \(\dot M\) into the disk at its external boundary. Dependence on the efficiency of mechanisms of angular momentum transport (connected with the magnetic field and turbulence) is weaker. If \(\dot M = {10^{ - 9}} - 3 \times {10^{ - 8}} {M_ \odot }/yr\), the disk around the black hole is a powerful source of X-radiation with hv ~ 1–10 keV and luminosity L ~ 1037–1038 erg s−1. If the flux of the accreting matter decreases, the effective temperature of radiation and the luminosity will drop. At the same time when \(\dot M >{10^{ - 9}}{M_ \odot }y{r^{ - 1}}\), the optical luminosity of the disk exceeds the solar one. The main contribution to the optical luminosity of the black hole is due to the re-radiation of that part of the X-ray and ultraviolet energy which is initially produced in the central high temperature regions of the disk and which is then absorbed by the low temperature outer regions. The optical radiation spectrum of such objects must be saturated by the broad emission recombination and resonance lines. Variability is connected with the character of the motion of the black hole and the gas flow in binary systems and possibly with eclipses. For well defined conditions, the hard radiation can evaporate the gas. This can counteract the matter inflow into the disk and lead to autoregulation of the accretion.

High mass x-ray binaries as a star formation rate indicator in distant galaxies

Based on CHANDRA observations of nearby starburst galaxies and RXTE/ASM, ASCA and MIR-KVANT/TTM studies of high mass X-ray binary (HMXB) populations in the Milky Way and Magellanic Clouds, we propose that the number and/or the collective X-ray luminosity of HMXBs can be used to measure the star formation rate (SFR) of a galaxy. We show that, within the accuracy of the presently available data, a linear relation between HMXB number and the star formation rate exists. The relation between SFR and collective luminosity of HMXBs is non-linear in the low SFR regime,

THE INTERACTION OF MATTER AND RADIATION IN A HOT-MODEL UNIVERSE.

L_X\propto \SFR^{\approx 1.7}

Cooling flows as a calorimeter of active galactic nucleus mechanical power

, and becomes linear only for sufficiently high star formation rate, when the total number of HMXB sources becomes sufficiently large. Such behaviour is caused by the fact, that we measure collective luminosity of a population of the discrete sources. Although more subtle SFR dependent effects are likely to exist, the data are broadly consistent with the existence of a universal luminosity function of HMXBs which can be roughly described as a power law with a differential slope of

X-ray emission from star-forming galaxies – I. High-mass X-ray binaries

\sim 1.6

The non-linear dependence of flux on black hole mass and accretion rate in core-dominated jets

, a cutoff at

The Milky Way in X-rays for an outside observer Log(N)-Log(S) and luminosity function of X-ray binaries from RXTE/ASM data

L_X \sim few \times 10^{40}

SMALL-SCALE FLUCTUATIONS OF RELIC RADIATION*

erg/sec and a normalisation proportional to the star formation rate. We apply our results to (spatially unresolved) starburst galaxies observed by CHANDRA at redshifts up to

Radiative feedback from quasars and the growth of massive black holes in stellar spheroids

z\sim 1

Supermassive black holes in elliptical galaxies: Switching from very bright to very dim

in the Hubble Deep Field North and show that the calibration of the collective luminosity of HMXBs as a SFR indicator based on the local sample agrees well with the SFR estimates obtained for these distant galaxies with conventional methods.