Three-dimensional Radiative Properties of Hot Accretion Flows onto the Galactic Centre Black Hole

Abstract

By solving radiative transfer equations, we examine three-dimensional radiative properties of a magnetohydrodynamic accretion flow model confronting with the observed spectrum of Sgr A*, in the vicinity of supermassive black hole at the Galactic centre. As a result, we find that the core of radio emission is larger than the size of the event horizon shadow and its peak location is shifted from the gravitational centre. We also find that the self-absorbed synchrotron emissions by the superposition of thermal electrons within a few tens of the Schwartzschild radius can account for low-frequency spectra below the critical frequency ${\nu }_c\approx 10^{12}$ Hz. Above the critical frequency, the synchrotron self-Compton emission by thermal electrons can account for variable emissions in recent near-infrared observations. In contrast to the previous study by Ohsuga et al. (2005), we found that the X-ray spectra by Bremsstrahlung emission of thermal electrons for the different mass accretion rates can be consistent with both the flaring state and the quiescent state of Sgr A* observed by {\it Chandra}.

8 pages, 4 figures, submitted to MNRAS

References in corpus (3)

• Event-horizon-scale structure in the supermassive black hole candidate at the Galactic Centre
• Images of the radiatively inefficient accretion flow surrounding a Kerr black hole: application in Sgr A*
• Accretion of Low Angular Momentum Material onto Black Holes: Radiation Properties of Axisymmetric MHD Flows

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• Measuring spin of a supermassive black hole at the Galactic centre -- Implications for a unique spin
• Multi-Epoch VERA Observations of Sagittarius A*: I. Images and Structural Variability
• Radiative Spectra from Disk Corona and Inner Hot Flow in Black Hole X-ray Binaries
• An Axiomatic Review of Israel-Stewart Hydrodynamics and Extended Irreversible Thermodynamics