On radiative acceleration in spine-sheath structured blazar jets
arXiv:1610.00717 · doi:10.1093/mnras/stw3002
Abstract
It has been proposed that blazar jets are structured, with a fast spine surrounded by a slower sheath or layer. This structured jet model explains some properties of their emission and morphology. Because of their relative motion, the radiation produced by one component is seen amplified by the other, thus enhancing the inverse Compton emission of both. Radiation is emitted anisotropically in the comoving frames, and causes the emitting plasma to recoil. As seen in the observer frame, this corresponds to a deceleration of the fastest component (the spine) and an acceleration of the slower one (the layer). While the deceleration of the spine has already been investigated, here we study for the first time the acceleration of the sheath and find self-consistent velocity profile solutions for both the spine and the sheath while accounting for radiative cooling. We find that the sheath can be accelerated to the velocities required by the observations if its leptons remain energetic in the acceleration region, assumed to be of the order of 100 Schwarzschild radii, demanding continuous injection of energetic particles in that region.
arXiv comment14 pages, 16 figures, submitted to MNRAS. Comments are welcome!
References in corpus (25)
- General Relativistic Magnetohydrodynamic Simulations of Jet Formation and Large-Scale Propagation from Black Hole Accretion Systems
- Structured jets in TeV BL Lac objects and radiogalaxies
- Afterglow lightcurves, viewing angle and the jet structure of gamma-ray bursts
- TeV BL Lac objects at the dawn of the Fermi era
- Parsec Scale Properties of Markarian 501
- Decelerating Flows in TeV Blazars: A Resolution to the BL Lac -- FR I Unification Problem
- Fermi Large Area Telescope Observations of Misaligned AGN
- Fermi/LAT broad emission line blazars
- Universal GRB jets from jet-cocoon interaction in massive stars
- Time Dependent Modeling of the Markarian 501 X-ray and TeV Gamma-Ray Data Taken During March and April, 1997
- The Jets of TeV Blazars at Higher Resolution: 43 GHz and Polarimetric VLBA Observations from 2005-2009
- Modelling the TeV gamma-ray spectra of two low redshift AGNs: Mkn 501 and Mkn 421
- The Parsec-Scale Structure and Jet Motions of the TeV Blazars 1ES 1959+650, PKS 2155-304, and 1ES 2344+514
- Energetics of Tev Blazars and Physical Constraints on their Emission Regions
- Structured jets in BL Lac objects: efficient PeV neutrino factories?
- The Parsec-Scale Jets of the TeV Blazars H 1426+428, 1ES 1959+650, and PKS 2155-304: 2001-2004
- Compton rockets and the minimum power of relativistic jets
- A sample of low-redshift BL Lacertae objects. II. EVN and MERLIN data and multi-wavelength analysis
- On the spine-layer scenario for the very high-energy emission of NGC 1275
- First-Epoch VLBA Imaging of Twenty New TeV Blazars
- The Sub-Luminal Parsec-scale Jet of Mkn 501
- Unveiling the nature of the gamma-ray emitting AGN PKS 0521-36
- 3C66B as a TeV radiogalaxy
- Gamma-Rays from Radio Galaxies: Fermi-Lat Observations
- Variation of bulk Lorentz factor in AGN jets due to Compton rocket in a complex photon field
Cited by in corpus (10)
- Off-axis prompt X-ray transients from the cocoon of short gamma-ray bursts
- Progress in unveiling extreme particle acceleration in persistent astrophysical jets
- An Introduction to Particle Acceleration in Shearing Flows
- Electron-proton co-acceleration on relativistic shocks in extreme-TeV blazars
- Magnetic Field Properties inside the Jet of Mrk 421: Multiwavelength Polarimetry Including the Imaging X-ray Polarimetry Explorer
- Particle Acceleration in Shearing Flows: Efficiencies and Limits
- Multi-Epoch VLBA Imaging of Twenty New TeV Blazars: Apparent Jet Speeds
- Testing emission models on the extreme blazar 2WHSP J073326.7+515354 detected at very high energies with the MAGIC telescopes
- Turbulence and Particle Acceleration in Shearing Flows
- Fast Optical Variability of the TeV Blazar PKS 1725+123 Observed by SVOM-VT and Insights from Multi-wavelength Follow-up Observations