Magnetic collimation of the relativistic jet in M 87

Gracia, José; Tsinganos, K.; Bogovalov, S. V.

doi:10.1051/0004-6361:200500175

Cited by 23 publications

(38 citation statements)

References 34 publications

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“…Gracia et al 8 used the shape of the fieldline separating the two region on the boundary surface to define the opening angle. As shown in this work, this particular fieldline and flux contours of synthetic maps are parallel for a wide range of models and distances along the jet.…”

Section: Discussionmentioning

confidence: 99%

“…Gracia et al 8 used the shape of the separating fieldline Ψ α to fit the observed opening angle as a function of distance from the core as collected by Ref. 1.…”

Section: Mhd Modelmentioning

confidence: 99%

“…All our models fail to fit the jet width at large distances close to the optical knot A at ∼ 900 pc. 8 Models with large initial opening angle, as model 1, have a hard time reproducing the opening angle distribution. It is in general very difficult to make the curve more concave.…”

Section: Mhd Modelmentioning

confidence: 99%

“…In a series of papers Gracia et al 6 and Tsinganos et al 7,8 tackled this problem and suggested a two-zone model. The model consists of an inner relativistic outflow, which is identified with the observed jet, and an outer non-relativistic disk-wind.…”

Section: Introductionmentioning

confidence: 99%

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MHD Models and Synthetic Synchrotron Maps for the Jet of M87

Gracia

Bogovalov²,

Tsinganos

2008

Int. J. Mod. Phys. D

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We present a self-consistent MHD model for the jet of M87. The model consist of two distinct zones: an inner relativistic outflow, which we identify with the observed jet, and an outer cold disk wind. While the former does not self-collimate efficiently due to its high effective inertia, the latter fulfills all the conditions for efficient collimation by the magneto-centrifugal mechanism. Given the right balance between the effective inertia of the inner flow and the collimation efficiency of the outer disk wind, the relativistic flow is magnetically confined into a well collimated beam for a wide range of parameters and matches the measurements of the opening angle of M87 over several orders of magnitude in spatial extent.In the second part of this work, we present synthetic synchrotron emission maps for our MHD models. In principle, the two-zone model can reproduce the morphological structure seen in radio observations, as central-peaked profiles across the jet close the the source, limb-bright further down the jet, and a bright knot close to the position of HST-1. However it is difficult to reconcile all features with a single set of parameters.

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Section: Discussionmentioning

confidence: 99%

“…Gracia et al 8 used the shape of the separating fieldline Ψ α to fit the observed opening angle as a function of distance from the core as collected by Ref. 1.…”

Section: Mhd Modelmentioning

confidence: 99%

Section: Mhd Modelmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

See 2 more Smart Citations

MHD Models and Synthetic Synchrotron Maps for the Jet of M87

Gracia

Bogovalov²,

Tsinganos

2008

Int. J. Mod. Phys. D

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“…The collimation of a central relativistic outflow can be provided by a non-relativistic MHD wind/jet produced by an accretion disk. Such a double jet structure was originally proposed by Sol et al (1989), and was investigated further by , Gracia et al (2005), and Beskin & Nokhrina (2006). The quasar systems with such efficiently collimated jets can be rare indeed due to the difficulties in developing the required large-scale poloidal magnetic fields in the geometrically thin accretion disks.…”

Section: The Spin Paradigmmentioning

confidence: 93%

Radio-loudness of active galaxies and the black hole evolution

Sikora

Stawarz

Lasota

2008

New Astronomy Reviews

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Active galactic nuclei (AGNs) form two distinct sequences on the radio-loudness -Eddington-ratio plane. The 'upper' sequence contains radio selected AGNs, the 'lower' sequence is composed mainly of optically selected AGNs. The sequences mark the upper bounds for the radio-loudness of two distinct populations of AGNs, hosted respectively by elliptical and disk galaxies. Both sequences show the same dependence of the radio-loudness on the Eddington ratio (an increase with decreasing Eddington ratio), which suggests that another parameter in addition to the accretion rate must play a role in determining the efficiency of jet production in AGNs. We speculate that this additional parameter is the spin of the black hole, assuming that black holes in giant elliptical galaxies have (on average) much larger spins than black holes in disc galaxies. Possible evolutionary scenarios leading to such a spin dichotomy are discussed. The galaxy-morphology related radio-dichotomy breaks down at high accretion rates where the dominant fraction of luminous quasars being hosted by giant ellipticals is radio quiet. This indicates that the production of powerful jets at high accretion rates is in most cases suppressed and, in analogy to X-ray binary systems (XRB) during high and very high states, may be intermittent. Such intermittency can be caused by switches between two different accretion modes, assuming that only during one of them an outflow from the central engine is sufficiently collimated to form a relativistic jet.

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Synthetic Jets - from Models to Observations and Back

Gracia

2009

Protostellar Jets in Context

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Magnetic collimation of the relativistic jet in M 87

Cited by 23 publications

References 34 publications

MHD Models and Synthetic Synchrotron Maps for the Jet of M87

MHD Models and Synthetic Synchrotron Maps for the Jet of M87

Radio-loudness of active galaxies and the black hole evolution

Synthetic Jets - from Models to Observations and Back

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