The structure of the jet in 3C 15 from multiband polarimetry

Dulwich, Fred; Worrall, D. M.; Birkinshaw, Mark; Padgett, C. A.; Perlman, Eric S.

doi:10.1111/j.1365-2966.2006.11242.x

Cited by 27 publications

(38 citation statements)

References 32 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…This can be achieved if an outer slower layer surrounds the central relativistic jet "spine" (Ghisellini et al 2005), since continuous electron acceleration acts at the boundary layer between jet sheath and "spine" (Stawarz & Ostrowski 2002). This kind of jet structure is supported by direct radio observations (Giroletti et al 2004) and leads to radial jet structure where the Lorentz factor decreases radially, as suggested both in microquasars (Meier 2003) and in AGN (Jester et al 2006;Dulwich et al 2007). This transverse jet stratification is also supported by models of jet launch scenarios (Koide et al 2001;McKinney 2006;Meliani et al 2006).…”

Section: Article Published By Edp Sciencesmentioning

confidence: 60%

Extragalactic jets with helical magnetic fields: relativistic MHD simulations

Keppens

Méliani

Holst³

et al. 2008

A&A

View full text Add to dashboard Cite

Context. Extragalactic jets are judged to harbor dynamically important, organized magnetic fields that presumably aid in the collimation of the relativistic jet flows. Aims. We here explore the morphology of AGN jets pervaded by helical field and flow topologies by means of grid-adaptive, highresolution numerical simulations. We concentrate on morphological features of the bow shock and the jet beam behind the Mach disk, for various jet Lorentz factors and magnetic field helicities. We investigate the influence of helical magnetic fields on jet beam propagation in an overdense external medium. We adopt a special relativistic magnetohydrodynamic (MHD) viewpoint on the shockdominated AGN jet evolution. Due to the adaptive mesh refinement (AMR), we can concentrate on the long-term evolution of kinetic energy-dominated jets, with beam-averaged Lorentz factor Γ 7, as they penetrate denser clouds. These jets have near-equipartition magnetic fields (with the thermal energy) and radially varying Γ(R) profiles within the jet radius R < R j maximally reaching Γ ∼ 22. Methods. We used the AMRVAC code, with a novel hybrid block-based AMR strategy, to compute ideal plasma dynamics in special relativity. We combined this with a robust second-order shock-capturing scheme and a diffusive approach to controlling magnetic monopole errors. Results. We find that the propagation speed of the bow shock systematically exceeds the value expected from estimates using beamaverage parameters, in accordance with the centrally-peaked Γ(R) variation. The helicity of the beam magnetic field is effectively transported down the beam, with compression zones between the diagonal internal cross-shocks showing stronger toroidal field regions. In comparison with equivalent low-relativistic jets (Γ 1.15), which get surrounded by cocoons with vortical backflows filled by mainly toroidal field, the high speed jets only demonstrate localized, strong toroidal field zones within the backflow vortical structures. These structures are ring-like due to our axisymmetry assumption and may further cascade to a smaller scale in 3D. We find evidence of a more poloidal, straight field layer, compressed between jet beam and backflows. This layer decreases the destabilizing influence of the backflow on the jet beam. In all cases, the jet beam contains rich cross-shock patterns, across which part of the kinetic energy gets transfered. For the high-speed reference jet considered here, significant jet deceleration only occurs beyond distances exceeding O(100R j ), as the axial flow can reaccelerate downstream to the internal cross shocks. This reacceleration is magnetically aided by field compression across the internal shocks that pinch the flow.

show abstract

Section: Article Published By Edp Sciencesmentioning

confidence: 60%

Extragalactic jets with helical magnetic fields: relativistic MHD simulations

Keppens

Méliani

Holst³

et al. 2008

A&A

View full text Add to dashboard Cite

show abstract

“…The X-ray emission associated with K2 peaks upstream of the radio. This has been seen elsewhere in X-ray synchrotron knots embedded in the jets of nearby radio galaxies, most notably in 3C 66B, Cen A, 3C 346, 3C 353 and possibly 3C 15 Hardcastle et al 2003;Kataoka et al 2008;Dulwich et al 2007). The spectral constraint on the X-ray emission from knot K2 is rather poor and alone does not rule out an origin as either inverse Compton emission from electrons of energies similar to those producing the radio synchrotron emission, or synchrotron radiation from highenergy electrons of steeper spectrum.…”

Section: Nonthermal X-ray Componentsmentioning

confidence: 73%

X-rays associated with the jet–cloud-interacting radio galaxy 3C 277.3 (Coma A): implications for energy deposition

Worrall

Birkinshaw

Young

2016

Mon. Not. R. Astron. Soc.

Self Cite

View full text Add to dashboard Cite

We report the discovery with Chandra of X-ray-emitting gas associated with the jet-cloud interaction in the radio galaxy 3C 277.3 (Coma A), a source that falls in the most important power range for radio-mode feedback in the Universe. This hot gas, heated by the jet, dominates the mass of the cloud which is responsible for an extreme projected deflection of the kpc-scale radio jet. Highly absorbed X-ray emission from the nucleus of 3C 277.3 confirms that the jet lies close to the plane of the sky and so has a large intrinsic deflection. We detect group gas on the scale of the radio lobes, and see X-ray cavities coincident with the brightest radio emission, with the lobes embraced by X-ray enhancements that we argue are the result of shocks. The anti-correlation between the locations of X-ray arms and Hα-emitting filaments that are believed to have originated from a merger with one or more gas-rich galaxies suggests that shocks advancing around the lobe are inhibited by the dense colder material. Synchrotron X-ray emission is detected from the upstream edge of a second bright radio knot. X-rays are also detected from the location where an undetected counterjet enters the northern radio hotspot. We suggest that these X-rays are synchrotron radiation from a shock in a small-scale substructure.

show abstract

“…The filament in NGC 315 differs both morphologically and in its polarization properties from features which have been identified as strong shocks, such as those producing bright X‐rays in M 87 (Perlman et al 1999) and 3C 15 (Dulwich et al 2007). The latter tend to show apparent magnetic fields transverse to the jet axis, whereas the filament has a primarily longitudinal field.…”

Section: Discussionmentioning

confidence: 98%

The inner jet of radio galaxy NGC 315 as observed with Chandra and the Very Large Array

Worrall

Birkinshaw

Laing

et al. 2007

Monthly Notices of the Royal Astronomical Society

Self Cite

View full text Add to dashboard Cite

We present Chandra X‐ray results for the jet, nucleus and gaseous atmosphere of NGC 315, a nearby radio galaxy whose jet kinematics are known through deep radio mapping. Diffuse X‐ray synchrotron emission is detected from the jet out to 30 arcsec from the nucleus, through regions both of fast bulk flow and deceleration. The X‐ray‐to‐radio flux ratio drops considerably where the flow decelerates, but the X‐ray and radio emissions show similar transverse extents throughout, requiring distributed particle acceleration to maintain the supply of X‐ray‐emitting electrons. A remarkable knotty filament within the jet is seen in both the radio and X‐ray, contributing roughly 10 per cent of the diffuse emission along its extent at both wavelengths. No completely satisfactory explanation for the filament is found, though its oscillatory appearance, roughly aligned magnetic field and requirements for particle acceleration, suggest that it is a magnetic strand within a shear layer between fast inner and slower outer flow.

show abstract

The structure of the jet in 3C 15 from multiband polarimetry

Cited by 27 publications

References 32 publications

Extragalactic jets with helical magnetic fields: relativistic MHD simulations

Extragalactic jets with helical magnetic fields: relativistic MHD simulations

X-rays associated with the jet–cloud-interacting radio galaxy 3C 277.3 (Coma A): implications for energy deposition

The inner jet of radio galaxy NGC 315 as observed with Chandra and the Very Large Array

Contact Info

Product

Resources

About