High-energy emission processes in M87

Jong, S. de; Beckmann, V.; Soldi, S.; Tramacere, A.; Gros, A.

doi:10.1093/mnras/stv927

Cited by 28 publications

(29 citation statements)

References 50 publications

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“…Our findings are in contrast to previous modelling efforts of M87 (e.g. Abdo et al 2009, de Jong et al 2015, who reproduced the SED of the source with a standard homogeneous one-zone SSC model. The parameters explored in both of these works require the plasma emitting in the core region to be strongly particle-dominated, with Ue/U b 100, in order to produce a meaningful high-energy flux; this is in contrast with VLBI data, which favours a magneticallydominated core (10 −1 < Ue/U b < 10 −4 , Kino et al 2014, Hada et al 2016.…”

Section: Discussioncontrasting

confidence: 99%

“…Despite such complex behaviour, the overall shape of the SED has been found in the past to be consistent with a standard one-zone synchrotron self-Compton (SSC) model (e.g. Abdo et al 2009, de Jong et al 2015, with the caveat that the implied bulk speed of the jet is far lower than that inferred from modelling blazar SEDs, in contrast with AGN unification models (Henri and Saugé 2006). One possible solution to this inconsistency, which is common for single-zone models, has been proposed by Tavecchio and Ghisellini (2008), who proposed that the jet is composed of an inner, relativistic spine and of a slower moving, outer sheath.…”

Section: Introductionsupporting

confidence: 57%

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The unique case of the AGN core of M87: a misaligned low power blazar?

Lucchini

Krauß

Markoff

2019

Monthly Notices of the Royal Astronomical Society

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M87 hosts one of the closest jetted active galactic nucleus (AGN) to Earth. Thanks to its vicinity and to the large mass of is central black hole, M87 is the only source in which the jet can be directly imaged down to near-event horizon scales with radio very large baseline interferometry (VLBI). This property makes M87 a unique source to isolate and study jet launching, acceleration and collimation. In this paper we employ a multi-zone model designed as a parametrisation of general relativistic magneto-hydrodynamics (GRMHD); for the first time we reproduce the jet's observed shape and multi-wavelength spectral energy distribution (SED) simultaneously. We find strong constraints on key physical parameters of the jet, such as the location of particle acceleration and the kinetic power. However, we under-predict the (unresolved) γ-ray flux of the source, implying that the high-energy emission does not originate in the magnetically-dominated inner jet regions. Our results have important implications both for comparisons of GRMHD simulations with observations, and for unified models of AGN classes.

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Section: Discussioncontrasting

confidence: 99%

Section: Introductionsupporting

confidence: 57%

The unique case of the AGN core of M87: a misaligned low power blazar?

Lucchini

Krauß

Markoff

2019

Monthly Notices of the Royal Astronomical Society

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“…This conclusion is similar to Yuan & Cui (2005); Wu et al (2007); Yuan et al (2009), where the X-ray emission should be dominated by the jet, not the ADAF, if the Eddington ratio is less than a critical value. It should be noted that our ADAF-jet model cannot explain the optical-UV emission, which may be contributed by the host galaxy (Nemmen et al 2014;de Jong et al 2015), and the multiwaveband flux variations may help to test this issue. We find that different BH spin parameters (a * = 0 − 0.99) and magnetic parameters (β = 0.5 − 0.9) yield an equivalent fit of the SED, but the accretion rate has to be decreased if high BH spin and stronger magnetic field (lower β) are adopted.…”

Section: Discussionmentioning

confidence: 96%

“…The acceleration zone of M87 jet may be co-spatial with the jet parabolic region, where the intrinsic jet velocity fields increase from ∼ 0.1 c at ∼ 10 2 R g to 1 c at ∼ 10 5 R g Asada et al 2014). The multi-wavelength nuclear SED of M87 has been extensively explored by both pure jet models (e.g., Dexter et al 2012;de Jong et al 2015;Prieto et al 2016) and ADAF+jet models (e.g., Di Matteo et al 2003;Yuan et al 2009;Broderick & Loeb 2009;Li et al 2009;Nemmen et al 2014;Mocibrodzka et al 2016), where the radio emission is produced by the jet in both models while the millimeter/sub-millimeter and X-ray emission can either come from the jet or ADAF. Apart from the continuum spectrum, linear polarization can be a diagnostic of the relativistic jets and accretion flows associated with BH systems.…”

Section: Introductionmentioning

confidence: 99%

An Accretion-Jet Model for M87: Interpreting the Spectral Energy Distribution and Faraday Rotation Measure

Feng

2016

ApJ

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M87 is arguably the best supermassive black hole (BH) to explore the jet and/or accretion physics due to its proximity and fruitful high-resolution multi-waveband observations. We model the multiwavelength spectral energy distribution (SED) of M87 core that observed at a scale of 0.4 arcsec (∼ 10 5 R g , R g is gravitational radius) as recently presented by Prieto et al. Similar to Sgr A*, we find that the millimeter bump as observed by Atacama Large Millimeter/submillimeter Array (ALMA) can be modeled by the synchrotron emission of the thermal electrons in advection dominated accretion flow (ADAF), while the low-frequency radio emission and X-ray emission may dominantly come from the jet. The millimeter radiation from ADAF dominantly come from the region within 10R g , which is roughly consistent with the recent very long baseline interferometry observations at 230 GHz. We further calculate the Faraday rotation measure (RM) from both ADAF and jet models, and find that the RM predicted from the ADAF is roughly consistent with the measured value while the RM predicted from the jet is much higher if jet velocity close to the BH is low or moderate (e.g., v jet 0.6 c). With the constraints from the SED modeling and RM, we find that the accretion rate close to the BH horizon isBondi accretion rate), where the electron density profile, n e ∝ r ∼−1 , in the accretion flow is consistent with that determined from X-ray observation inside the Bondi radius and recent numerical simulations.

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“…[19]), and we assume respectively for the BH spin and the external magnetic field, ca/(G M) = 0.9 and B 0 = 50 G. The magnetic field has been fixed to explain the observed high-energy luminosity which is few × 10 42 erg s −1 (e.g. [20,21]).…”

Section: Specific Quantitative Examplesmentioning

confidence: 99%

The blackholic quantum

Rueda

Ruffini

2020

Eur. Phys. J. C

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We show that the high-energy emission of GRBs originates in the inner engine: a Kerr black hole (BH) surrounded by matter and a magnetic field B 0 . It radiates a sequence of discrete events of particle acceleration, each of energy E =h Ω eff , the blackholic quantum,+ ) and r + are the BH mass, angular momentum per unit mass, angular velocity and horizon; m n is the neutron mass, m Pl , λ Pl =h/(m Pl c) and ρ Pl = m Pl c 2 /λ 3 Pl , are the Planck mass, length and energy density. The timescale of each process is τ el ∼ Ω −1 + . We show an analogy with the Zeeman and Stark effects, properly scaled from microphysics to macrophysics, that allows us to define the BH magneton, µ BH = (m Pl /m n ) 4 (c a/G M)eh/(Mc). We give quantitative estimates for GRB 130427A adopting M = 2.3 M ⊙ , c a/(G M) = 0.3 and B 0 = 2.9 × 10 14 G. Each emitted quantum, E ∼ 10 44 erg, extracts only 10 −9 times the BH rotational energy, guaranteeing that the process can be repeated for thousands of years. The inner engine can also work in AGN as we here exemplified for the supermassive BH at the center of M87.

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High-energy emission processes in M87

Cited by 28 publications

References 50 publications

The unique case of the AGN core of M87: a misaligned low power blazar?

The unique case of the AGN core of M87: a misaligned low power blazar?

An Accretion-Jet Model for M87: Interpreting the Spectral Energy Distribution and Faraday Rotation Measure

The blackholic quantum

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