اشترك بالحزمة الذهبية واحصل على وصول غير محدود شمرا أكاديميا
تسجيل مستخدم جديدBlack Hole Winds
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We show that black holes accreting at or above the Eddington rate probably produce winds which are optically thick in the continuum, whether in quasars or X-ray binaries. The photospheric radius and outflow speed are proportional to mo^2 and mo^-1 respectively, where mo is the mass outflow rate. The outflow momentum rate is always of order L_Edd/c. Blackbody emission from these winds may provide the big blue bump in some quasars and AGN, as well as ultrasoft X-ray components in ULXs.
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We want to test if self-similar magneto-hydrodynamic (MHD) accretion-ejection models can explain the observational results for accretion disk winds in BHBs. In our models, the density at the base of the outflow, from the accretion disk, is not a free
parameter, but is determined by solving the full set of dynamical MHD equations without neglecting any physical term. Different MHD solutions were generated for different values of (a) the disk aspect ratio ($varepsilon$) and (b) the ejection efficiency ($p$). We generated two kinds of MHD solutions depending on the absence (cold solution) or presence (warm solution) of heating at the disk surface. The cold MHD solutions are found to be inadequate to account for winds due to their low ejection efficiency. The warm solutions can have sufficiently high values of $p (gtrsim 0.1)$ which is required to explain the observed physical quantities in the wind. The heating (required at the disk surface for the warm solutions) could be due to the illumination which would be more efficient in the Soft state. We found that in the Hard state a range of ionisation parameter is thermodynamically unstable, which makes it impossible to have any wind at all, in the Hard state. Our results would suggest that a thermo-magnetic process is required to explain winds in BHBs.
The formation of supermassive black holes is still an outstanding question. In the quasi-star scenario, black hole seeds experience an initial super-Eddington growth, that in less than a million years may leave a $10^4-10^5$ M$_{odot}$ black hole at
the centre of a protogalaxy at $z sim 20-10$. Super-Eddington accretion, however, may be accompanied by vigorous mass loss that can limit the amount of mass that reaches the black hole. In this paper, we critically assess the impact of radiative driven winds, launched from the surface of the massive envelopes from which the black hole accretes. Solving the full wind equations coupled with the hydrostatic structure of the envelope, we find mass outflows with rates between a few tens and $10^4$ M$_{odot}$ yr$^{-1}$, mainly powered by advection luminosity within the outflow. We therefore confirm the claim by Dotan, Rossi & Shaviv (2011) that mass losses can severely affect the black hole seed early growth within a quasi-star. In particular, seeds with mass $>10^4$ M$_{odot}$ can only form within mass reservoirs $ gtrsim 10^7$ M$_{odot}$, unless they are refilled at huge rates ($ gtrsim 100$ M$_{odot}$ yr$^{-1}$). This may imply that only very massive halos ($>10^9$ M$_{odot}$) at those redshifts can harbour massive seeds. Contrary to previous claims, these winds are expected to be relatively bright ($10^{44}-10^{47}$ erg s$^{-1}$), blue ($T_{rm eff} sim 8000$ K) objects, that while eluding the Hubble Space Telescope, could be observed by the James Webb Space Telescope.
Black hole accretion disks appear to produce invariably plasma outflows that result in blue-shifted absorption features in their spectra. The X-ray absorption-line properties of these outflows are quite diverse, ranging in velocity from non-relativis
tic ($sim 300$ km/sec) to sub-relativistic ($sim 0.1c$ where $c$ is the speed of light) and a similarly broad range in the ionization states of the wind plasma. We report here that semi-analytic, self-similar magnetohydrodynamic (MHD) wind models that have successfully accounted for the X-ray absorber properties of supermassive black holes, also fit well the high-resolution X-ray spectrum of the accreting stellar-mass black hole, GRO J1655-40. This provides an explicit theoretical argument of their MHD origin (aligned with earlier observational claims) and supports the notion of a universal magnetic structure of the observed winds across all known black hole sizes.
We present a study of the mechanical power generated by both winds and jets across the black hole mass scale. We begin with the study of ionized X-ray winds and present a uniform analysis using Chandra grating spectra. The high quality grating spectr
a facilitate the characterization of the outflow velocity, ionization and column density of the absorbing gas. We find that the kinetic power of the winds scales with increasing bolometric luminosity as log(L_wind) propto (1.58 pm 0.07) log(L_Bol). This means that SMBH may be more efficient than stellar-mass black holes in launching winds. In addition, the simplicity of the scaling may suggest common driving mechanisms across the mass scale. For comparison, we next examine jet production, estimating jet power based on the energy required to inflate local bubbles. The jet relation is log(L_Jet)propto (1.18pm0.24) log(L_Bol). The energetics of the bubble associated with Cygnus X-1 are particularly difficult to determine, and the bubble could be a background SNR. If we exclude Cygnus X-1, then the jets follow a consistent relation to the winds within errors but with a higher normalization, log(L_Jet) propto (1.34 pm 0.50) log(L_Bol). The formal consistency in the wind and jet scaling relations suggests that a common launching mechanism may drive both flows; magnetic processes are viable possibilities. We also examine winds with especially high velocities, v > 0.01c. These ultra-fast outflows tend to resemble the jets more than the winds, indicating we may be observing a regime in which winds become jets. This study allows for the total power from black hole accretion, both mechanical and radiative, to be characterized in a simple manner and suggests a possible connection between winds and jets. Finally, we find at low Eddington fractions, the jet power is dominant, and at high Eddington fractions the wind power is dominant.
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perhaps during the quasar phase of rapid accretion onto a supermassive black hole, an unknown mechanism must remove or heat subsequently accreted gas from stellar mass loss or mergers that would otherwise cool to form stars. Energy output from a black hole accreting at a low rate has been proposed, but observational evidence for this in the form of expanding hot gas shells is indirect and limited to radio galaxies at the centers of clusters, which are too rare to explain the vast majority of the quiescent population. Here we report bisymmetric emission features co-aligned with strong ionized gas velocity gradients from which we infer the presence of centrally-driven winds in typical quiescent galaxies that host low-luminosity active nuclei. These galaxies are surprisingly common, accounting for as much as $10%$ of the population at $M_* sim 2 times 10^{10}~ M_{odot}$. In a prototypical example, we calculate that the energy input from the galaxys low-level active nucleus is capable of driving the observed wind, which contains sufficient mechanical energy to heat ambient, cooler gas (also detected) and thereby suppress star formation.
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