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Sgr A* represents a unique laboratory for the detailed study of accretion processes around a low-luminosity supermassive black hole (SMBH). Recent X-ray observations have allowed for spatially resolved modelling of the emission from the accretion flow around the SMBH, placing tight constraints on the flux and spectral shape of the accretion from the inner region with r < 103 R g, where R g ≡ GM BH/ c 2 is the gravitational radius of the black hole of mass M BH. We present here the first modelling of the multiband spectral energy distribution (SED) of this inner region to better constrain the physical condition of the innermost accretion flow. Our modelling uses the Markov chain Monte Carlo method to fit the SED, accounting for the limitations on the accretion rate at the outer radius of 103 R g from the earlier works and the domination of the accretion flow within 30 R g to the sub-mm bump. It is found that the fitting results of the outflow index could be very different. If only the most luminous part of the SED, the sub-mm bump, is considered, the outflow index is about 0, while if low-frequency radio data and X-ray data are also included, the outflow index could be 0.37 or even higher. The great difference of the fitting results indicates that the outflow index should be variable along radius, with a strong outflow in the outer region and a weak outflow in the innermost region. Such a weak outflow agrees with numerical simulations and makes it possible to explain the multiband SED even better. [ABSTRACT FROM AUTHOR]

Many analyses have concluded that the accretion disc sizes measured from the microlensing variability of quasars are larger than the expectations from the standard thin disc theory by a factor of ∼4. We propose a simple model by invoking a strong wind from the disc to flatten its radial temperature profile, which can then reconcile the size discrepancy problem. This wind model has been successfully applied to several microlensed quasars with a wind strength s ≲ 1.3 by only considering the inward decreasing of the mass accretion rate [where s is defined through |$\dot{M}(R)\propto ({R}/{R_{0}})^{s}$| ]. After further incorporating the angular momentum transferred by the wind, our model can resolve the disc size problem with an even lower wind parameter. The corrected disc sizes under the wind model are correlated with black hole masses with a slope in agreement with our modified thin disc model. [ABSTRACT FROM AUTHOR]

The giant X-ray bump of GRB 121027A observed by Swift is different from the typical X-ray flares in gamma-ray bursts. The observed structural variability in the rise and decay phases of the bump has four components. Of these four components, only the data in the bump from about 5300 to about 6100 s is of good enough quality to be analysed using the stepwise filter correlation method. A $86^{+5.9}_{-9.4} \rm s$ periodic oscillation is postulated, which is confirmed by the Lomb–Scargle method. A jet precession model is proposed to account for this variability. [ABSTRACT FROM AUTHOR]