Fundamental Plane of Black Hole Activity in the Quiescent Regime

Xie, Fu-Guo; Yuan, Feng

doi:10.3847/1538-4357/aa5b90

Cited by 29 publications

(45 citation statements)

References 110 publications

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“…There is then a remarkable area which is potentially capable to unify very different issues of high energy astrophysics connecting X-ray emission, black hole (BH) physics related to accretion processes, and galaxy mergers see, e.g., [2] and [3,4]. The origin of X-ray emission in BH environments is especially viewed as accretion related, and possibly a bridge between galaxy and a galactic BH activity keeping fingerprints of galaxy mergers [5,6,7,8,9,4,10]. There are various studies of the X-ray emission profile, and more generally jet emission, using more or less the Send offprint requests to: 1 For example from XMM-Newton: https://www.cosmos.esa.…”

Section: Introductionmentioning

confidence: 99%

RADs energetics and constraints on emerging tori collisions around super-massive Kerr black holes

Pugliese

Stuchlík

2019

Eur. Phys. J. C

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We provide constraints on possible configurations and interactions of two coplanar tori orbiting a central Kerr black hole (BH), in dependence on its dimensionless spin. The two-tori configurations can be directly linked to the current models featuring the obscuration of galactic BH X-ray emission. The emergence of each torus instability phases is discussed and tori collision has been also investigated. The first simple evaluation of the center-of-mass energy proves that collision-energy-efficiency increases with the dimensionless BH spin. We explore the phenomenological aspects of the corotating and counterrotating tori by analyzing properties of the orbiting toroidal configurations related to the fluid enthalpy flux, the mass-flux, the mass-accretion-rates, and the cusp luminosity in the two cases of corotating and counterrotating fluids in dependence on the SMBH spin. The analysis resulted ultimately in a comparative investigation of the properties of corotating versus counterrotating tori, demonstrating that two accretion tori can orbit around the central Kerr attractor only under very specific conditions. Our results also demonstrate that the dynamics of the unstable phases of these double tori systems is significant for the high energy phenomena which could be observable in the X-ray emission and extremely energetic phenomena in active galactic nuclei and quasar.

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Section: Introductionmentioning

confidence: 99%

RADs energetics and constraints on emerging tori collisions around super-massive Kerr black holes

Pugliese

Stuchlík

2019

Eur. Phys. J. C

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“…Therefore, they concluded that the fundamental plane should be most suitable for radiatively inefficient BH sources. Another form of the fundamental plane for radiatively efficient BHs is established by Dong et al (2014) and Xie & Yuan (2017).…”

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confidence: 99%

A universal scaling law of black hole activity including gamma-ray bursts

Wang

Dai

2017

Monthly Notices of the Royal Astronomical Society

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Previous works show that a correlation among radio luminosity, X-ray luminosity, and black hole (BH) mass from stellar-mass BHs in X-ray binaries to supermassive BHs in active galactic nuclei (AGNs), which leads to the so-called fundamental plane of BH activity. However, there are two competing explanations for this fundamental plane, including the jet-dominated model and the disk-jet model. Thus, the physical origin of this fundamental plane remains unknown. In this paper, we show that the X-ray luminosities, radio luminosities and BH masses of gamma-ray bursts (GRBs) and M82 X-1 also show a similar distribution. The universal scaling law among stellar-mass, intermediate and supermassive BH systems, together with the fact that radio and X-ray emission of GRBs originates from relativistic jets, reveals that the fundamental plane of BH activity is controlled by a jet, i.e., the radio and X-ray emission is mainly from the jet. Our work also suggests that the jets are scale-invariant with respect to the BH mass.

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“…However, different correlation slope p is reported in some specified systems, e.g. the radio-loud AGNs (Wang et al 2006;Panessa et al 2007;Li et al 2008), the narrow-line Seyfert 1 galaxies (Yao et al 2018), and the faint/quiescent AGNs (Yuan et al 2009b;Xie & Yuan 2017, but see Mezcua et al 2018). 3 Even within its typical dynamical range, sources with clear deviations to the standard RX correlation are observed in both BHBs (so called "outliers" for BHBs, e.g., Corbel et al 2004;Coriat et al 2011;Jonker et al 2012;Brocksopp et al 2013) and AGNs (e.g., Bell et al 2011;King et al 2011King et al , 2013.…”

Section: Introductionmentioning

confidence: 95%

“…Physically, the standard RX correlation provides strong evidence for a tight connection between the hot X-ray emitting source (usually a hot accretion flow), and the radio 2 A slight offset in the normalization among the full and failed (defined as the case of no transition into the soft state) outbursts are observed in GX 339-4 (Fürst et al 2015). 3 Quiescent BHBs seem to follow the standard RX correlation Plotkin et al 2017), maybe because they are still not dim enough in these observations (e.g., discussions in Xie & Yuan 2017, and a hint in Dincer et al 2018). source (usually a continuous jet), and it is understood under the coupled accretion-jet model, where a scale-invariant jet model is considered (e.g., Heinz & Sunyaev 2003;Merloni et al 2003;Heinz 2004;Yuan & Cui 2005;Xie & Yuan 2016). The physics behind the hybrid RX correlation, as well as its connection to the standard one, on the other hand, remain unclear.…”

Section: Introductionmentioning

confidence: 99%

Radio/X-Ray Correlation in the Mini-outbursts of Black Hole X-Ray Transient GRS 1739–278

Xie

Yan

2020

ApJ

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We present quasi-simultaneous radio and X-ray observations of the black hole X-ray binary GRS 1739-278 of its 2015-2016 mini-outbursts, i.e. between 2015 June 10 and 2016 October 31, with the X-ray-to-radio time interval being less than one day. The monitor campaign was run by Swift in the X-rays and by JVLA in the radio (at both 5 GHz and 8 GHz). We find that the brightest radio emission is actually achieved during the soft sate, and the spectrum is marginally optically-thick with the spectral index α ≈ −0.28 ± 0.17 (flux F ν ∝ ν α ). For the radio emission in the hard state, we find a large diversity in the spectral index, i.e. a majority of radio spectra are optically-thick with −0.5 α 0.5, while a few are optically-thin, with α being lower than −1 in certain cases. We then investigate the correlation between the luminosities in radio (monochromatic at 5 GHz, L R ) and 1-10 keV X-rays (L X ) during the hard state. We find that for more than two orders of magnitude variation in the X-ray luminosity, this source exhibits a flat correlation with p ≈ 0.16 (in the form of L R ∝ L p X ), i.e. it belongs to the "outlier" (to the standard correlation with p ≈ 0.6) category that may follow a hybrid correlation. Both the slope and the corresponding luminosity range agree well with those in H1743-322, the prototype of the hybrid correlation. Theoretical implications of our results are discussed.

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Fundamental Plane of Black Hole Activity in the Quiescent Regime

Cited by 29 publications

References 110 publications

RADs energetics and constraints on emerging tori collisions around super-massive Kerr black holes

RADs energetics and constraints on emerging tori collisions around super-massive Kerr black holes

A universal scaling law of black hole activity including gamma-ray bursts

Radio/X-Ray Correlation in the Mini-outbursts of Black Hole X-Ray Transient GRS 1739–278

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