The Universal “Heartbeat” Oscillations in Black Hole Systems Across the Mass-Scale

Wu, Qingwen; Grzȩdzielski, Mikołaj; Janiuk, Agnieszka; Gu, Wei‐Min; Dong, Ai‐Jun; Cao, Xuejun; You, Bei; Yan, Zhen

doi:10.3847/1538-4357/833/1/79

Cited by 32 publications

(45 citation statements)

References 46 publications

(55 reference statements)

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“…Thus, by confronting the model predictions with observed flares, we can put constraints on those built-in assumptions. The attractiveness of the radiation pressure instability as a mechanism to explain various phenomena across the whole black hole mass scale has been outlined by Wu et al (2016). In the present paper we expand this work by making a systematic study showing how the model parameters modify the local stability curve and global disk behaviour.…”

Section: Introductionmentioning

confidence: 72%

“…The observation presented in Fig. 12 and our numerical model were presented also in Wu et al (2016). In that article, the source HLX-1 was also compared to a broad ensemble of XRBs and AGNs.…”

Section: Hlx-1 Mass Determinationmentioning

confidence: 84%

“…Thus the overall disk emission may not be significantly modified for the outer radii, and the hottest tail can still extend up to the soft X-ray band. A factor of 5 qualitatively accounts for that trend (Maccarone et al 2003;Wu et al 2016). In fact our method, which determines the mass, accretion rate, and parameters µ and α does not depend on the scaling factor connected with the bolometric luminosity and its validity is only indicative, in contradiction to P, A, and ∆ estimations, that are the outcome of the non-linear internal dynamics of the accretion disk and give independent approximations on the disk parameters (e.g.…”

Section: Hlx-1 Mass Determinationmentioning

confidence: 90%

“…In that article, the source HLX-1 was also compared to a broad ensemble of XRBs and AGNs. In Wu et al (2016) we already outlined the method presented in the current work, but here we present much a more detailed description of our generalised model. In particular, we tested the large parameter space of our computations, and verified their influence on the observable characteristics of the sources.…”

Section: Hlx-1 Mass Determinationmentioning

confidence: 99%

“…The above Equation is a generalised version of the results from Czerny et al (2009) and Wu et al (2016). In Fig.…”

Section: Disk Instability In Supermassive Black Holesmentioning

confidence: 99%

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Modified viscosity in accretion disks

Grzȩdzielski

Janiuk

2017

A&A

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Aims Black holes (BHs) surrounded by accretion disks are present in the Universe at different scales of masses, from microquasars up to the active galactic nuclei (AGNs). Since the work of Shakura and Sunyaev (1973) and their α-disk model, various prescriptions for the heat-production rate are used to describe the accretion process. The current picture remains ad hoc due the complexity of the magnetic field action. In addition, accretion disks at high Eddington rates can be radiation-pressure dominated and, according to some of the heating prescriptions, thermally unstable. The observational verification of their resulting variability patterns may shed light on both the role of radiation pressure and magnetic fields in the accretion process. Methods We compute the structure and time evolution of an accretion disk, using the code GLADIS (which models the global accretion disk instability). We supplement this model with a modified viscosity prescription, which can to some extent describe the magnetisation of the disk. We study the results for a large grid of models, to cover the whole parameter space, and we derive conclusions separately for different scales of black hole masses, which are characteristic for various types of cosmic sources. We show the dependencies between the flare or outburst duration, its amplitude, and period, on the accretion rate and viscosity scaling. Results We present the results for the three grids of models, designed for different black hole systems (X-ray binaries, intermediate mass black holes, and galaxy centres). We show that if the heating rate in the accretion disk grows more rapidly with the total pressure and temperature, the instability results in longer and sharper flares. In general, we confirm that the disks around the supermassive black holes are more radiation-pressure dominated and present relatively brighter bursts. Our method can also be used as an independent tool for the black hole mass determination, which we confront now for the intermediate black hole in the source HLX-1. We reproduce the light curve of the HLX-1 source. We also compare the duration times of the model flares with the ages and bolometric luminosities of AGNs. Conclusions With our modelling, we justify the modified µ-prescription for the stress tensor τ rφ in the accretion flow in microquasars. The discovery of the Ultraluminous X-ray source HLX-1, claimed to be an intermediate black hole, gives further support to this result. The exact value of the µ parameter, as fitted to the observed light curves, may be treated as a proxy for the magnetic field strength in the accretion flow in particular sources, or their states.

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Section: Introductionmentioning

confidence: 72%

Section: Hlx-1 Mass Determinationmentioning

confidence: 84%

Section: Hlx-1 Mass Determinationmentioning

confidence: 90%

Section: Hlx-1 Mass Determinationmentioning

confidence: 99%

“…The above Equation is a generalised version of the results from Czerny et al (2009) and Wu et al (2016). In Fig.…”

Section: Disk Instability In Supermassive Black Holesmentioning

confidence: 99%

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Modified viscosity in accretion disks

Grzȩdzielski

Janiuk

2017

A&A

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Accretion disks, quasars and cosmology: meandering towards understanding

Czerny

Cao

Jaiswal

et al. 2023

Astrophys Space Sci

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As Setti and Woltjer noted back in 1973, one can use quasars to construct the Hubble diagram; however, the actual application of the idea was not that straightforward. It took years to implement the proposition successfully. Most ways to employ quasars for cosmology now require an advanced understanding of their structure, step by step. We briefly review this progress, with unavoidable personal biases, and concentrate on bright unobscured sources. We will mention the problem of the gas flow character close to the innermost stable circular orbit near the black hole, as discussed five decades ago. This problem later led to the development of the slim disk scenario and is recently revived in the context of Magnetically Arrested Disks (MAD) and Standard and Normal Evolution (SANE) models. We also discuss the hot or warm corona issue, which is still under debate and complicates the analysis of X-ray reflection. We present the scenario of the formation of the low ionization part of the Broad Line Region as a failed wind powered by radiation pressure acting on dust (Failed Radiatively Driven Dusty Outflow – FRADO). Next, we examine the cosmological constraints currently achievable with quasars, primarily concentrating on light echo methods (continuum time delays and spectral-line time delays to the continuum) that are (or should be) incorporating the progress mentioned above. Finally, we briefly discuss prospects in this lively subject area.

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The Milky Way’s Supermassive Black Hole: How Good a Case Is It?

Eckart

Hüttemann²,

Kiefer³

et al. 2017

Found Phys

117

105

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The compact and, with 4.3±0.3×106 M ⊙ , very massive object located at the center of the Milky Way is currently the very best candidate for a supermassive black hole (SMBH) in our immediate vicinity. The strongest evidence for this is provided by measurements of stellar orbits, variable X-ray emission, and strongly variable polarized near-infrared emission from the location of the radio source Sagittarius A* (SgrA*) in the middle of the central stellar cluster. Simultaneous near-infrared and X-ray observations of SgrA* have revealed insights into the emission mechanisms responsible for the powerful near-infrared and X-ray flares from within a few tens to one hundred Schwarzschild radii of such a putative SMBH at the center of the Milky Way. If SgrA* is indeed a SMBH it will, in projection onto the sky, have the largest event horizon and will certainly be the first and most important target of the Event Horizon Telescope (EHT) Very Long Baseline Interferometry (VLBI) observations currently being prepared. These observations in combination with the infrared interferometry experiment GRAVITY at the Very Large Telescope Interferometer (VLTI) and other experiments across the electromagnetic spectrum might yield proof for the presence of a black hole at the center of the Milky Way. The large body of evidence continues to discriminate the identification of SgrA* as a SMBH from alternative possibilities. It is, however, unclear when the ever mounting evidence for SgrA* being associated with a SMBH will suffice as a convincing proof. Additional compelling evidence may come from future gravitational wave observatories. This manuscript reviews the observational facts, theoretical grounds and conceptual aspects for the case of SgrA* being a black hole. We treat theory and observations in the framework of the philosophical discussions about "(Anti)Realism and Underdetermination", as this line of arguments allows us to describe the situation in observational astrophysics with respect to supermassive black holes. Questions concerning the existence of supermassive black holes and in particular SgrA* are discussed using causation as an indispensable element. We show that the results of our investigation are convincingly mapped out by this combination of concepts.

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The Universal “Heartbeat” Oscillations in Black Hole Systems Across the Mass-Scale

Cited by 32 publications

References 46 publications

Modified viscosity in accretion disks

Modified viscosity in accretion disks

Accretion disks, quasars and cosmology: meandering towards understanding

The Milky Way’s Supermassive Black Hole: How Good a Case Is It?

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