Constraint on the black hole spin of M87 from the accretion-jet model

Feng, Jian‐Chao; Wu, Qingwen

doi:10.1093/mnras/stx1283

Cited by 36 publications

(28 citation statements)

References 83 publications

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“…The 1σ error in this fit corresponds to the observed width of the asymmetric bright ring on the M87* image[1][2][3][4][5][6]. The derived value of the M87* spin is in a general agreement with the other similar estimations[44][45][46][47][48][49][50][51][52]. See inFigure 6the superposition of the M87* image and the modelled image of the thin accretion disk in the case of a = 0.75.FIG.…”

supporting

confidence: 76%

The Brightest Point in Accretion Disk and Black Hole Spin: Implication to the Image of Black Hole M87*

Dokuchaev

Nazarova

2019

Universe

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We propose the simple new method for extracting the value of the black hole spin from the direct high-resolution image of black hole by using a thin accretion disk model. In this model the observed dark region on the first image of the supermassive black hole in the galaxy M87, obtained by the Event Horizon Telescope, is a silhouette of the black hole event horizon. The outline of this silhouette is the equator of the event horizon sphere. The dark silhouette of the black hole event horizon is placed within the expected position of the black hole shadow, which is not revealed on the first image. We calculated numerically the relation between the observed position of the black hole silhouette and the brightest point in the thin accretion disk, depending on the black hole spin. From this relation we derive the spin of the supermassive black hole M87*, a = 0.75 ± 0.15.

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supporting

confidence: 76%

The Brightest Point in Accretion Disk and Black Hole Spin: Implication to the Image of Black Hole M87*

Dokuchaev

Nazarova

2019

Universe

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“…The spin bounds from this work encompass-but are less restrictive-than previous estimates in the literature based on semi-analytic spectral fits (Feng & Wu 2017), TeV pair production (Li et al 2009) and jet wobbling (Sob'yanin 2018).…”

Section: Discussionmentioning

confidence: 67%

The Spin of M87*

Nemmen

2019

ApJL

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Now that the mass of the central black hole in the galaxy M87 has been measured with great precision using different methods, the remaining parameter of the Kerr metric that needs to be estimated is the spin a * . We have modeled measurements of the average power of the relativistic jet and an upper limit to the mass accretion rate onto the black hole with general relativistic magnetohydrodynamic models of jet formation. This allows us to derive constraints on a * and the black hole magnetic flux φ. We find a lower limit on M87*'s spin and magnetic flux of |a * | ≥ 0.4 and φ 6 in the prograde case, and |a * | ≥ 0.5 and φ 10 in the retrograde case, otherwise the black hole is not able to provide enough energy to power the observed jet. These results indicate that M87* has a moderate spin at minimum and disfavor a variety of models typified by low values of φ known as "SANE", indicating that M87* prefers the magnetically arrested disk state. We discuss how different estimates of the jet power and accretion rate can impact a * and φ.

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“…In this case, hot gas/corona above the thin disc may help launching outflows/jets Cao 2014), though the field is not formed through "coronal mechanism". For those less powerful jets in radio galaxies, there is evidence that the jets may be closely related to the ADAFs surrounding spinning black holes (e.g., Wu, Yan, & Yi 2013;Feng & Wu 2017). …”

Section: Resultsmentioning

confidence: 99%

The power of the jets accelerated by the coronal magnetic field

Cao

2017

Monthly Notices of the Royal Astronomical Society

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It was suggested that the large scale magnetic field can be dragged inwards efficiently by the corona above the disc, i.e., the so called "coronal mechanism" (Beckwith, Hawley, & Krolik 2009), which provides a way to solve the difficulty of field advection in a geometrically thin accretion disc. In this case, the magnetic pressure should be lower than the gas pressure in the corona. We estimate the maximal power of the jets accelerated by the magnetic field advected by the corona. The Blandford-Payne (BP) jet power is found always to be higher than the Blandford-Znajek (BZ) jet power, except for a rapidly spinning black hole with a 0.8. The maximal jet power is always low, less than 0.05 Eddington luminosity, even for an extreme Kerr black hole, which is insufficient for the observed strong jets in some blazars with jet power ∼ 0.1 − 1 Eddington luminosity (or even higher). It implies that these powerful jets cannot be accelerated by the coronal field. We suggest that, the magnetic field dragged inward by the accretion disc with magnetically outflows may accelerate the jets (at least for the most powerful jets, if not all) in the blazars.

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Constraint on the black hole spin of M87 from the accretion-jet model

Cited by 36 publications

References 83 publications

The Brightest Point in Accretion Disk and Black Hole Spin: Implication to the Image of Black Hole M87*

The Brightest Point in Accretion Disk and Black Hole Spin: Implication to the Image of Black Hole M87*

The Spin of M87*

The power of the jets accelerated by the coronal magnetic field

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