Adiabatic relativistic models for the jets in the radio galaxy 3C 31

Laing, R. A.; Bridle, A. H.

doi:10.1111/j.1365-2966.2004.07471.x

Cited by 42 publications

(72 citation statements)

References 24 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…-The longitudinal/toroidal field ratio decreases with distance from the nucleus, qualitatively as expected in an expanding, decelerating flow. -The evolution of the field-component ratios is not, however, consistent with flux freezing in a laminar velocity field of the type we infer, even if we include the effects of velocity shear (Laing & Bridle 2004). …”

Section: Field Configurationsmentioning

confidence: 85%

Magnetic fields in jets: ordered or disordered?

Laing¹,

Canvin²,

Bridle³

2006

Astron Nachr

Self Cite

View full text Add to dashboard Cite

Abstract. The question of the degree of order in the magnetic fields of relativistic jets is important to any understanding of their production. Both vector-ordered (e.g. helical) and disordered, but anisotropic fields can produce the high observed degrees of polarization. We outline our models of jets in FR I radio galaxies as decelerating relativistic flows. We then present theoretical calculations of the synchrotron emission from different field configurations and compare them with observed emission from FR I jets. We show that large-scale helical fields (with significant poloidal and toroidal components) are inconsistent with observations. The combination of an ordered toroidal and disordered poloidal component is consistent with our data, as is an entirely disordered field. Jets must also contain small, but significant amounts of radial field.

show abstract

Section: Field Configurationsmentioning

confidence: 85%

Magnetic fields in jets: ordered or disordered?

Laing¹,

Canvin²,

Bridle³

2006

Astron Nachr

Self Cite

View full text Add to dashboard Cite

show abstract

“…This might provide a more natural explanation for the deceleration that is necessary to account for the changing X-ray : radio ratios along some extragalactic jets, including 3C 273's (see Hardcastle [2006] and in particular Marshall et al [2006] for the deceleration of this jet implied by a one-zone beamed IC model). The FR I flow modeling by Laing & Bridle (2004), Canvin et al (2005) shows that these jets decollimate as they decelerate, presumably by entrainment, while no sign of decollimation is observed in 3C 273 and other high-power jets.…”

Section: Jet Deceleration In a Two-zone Ic-cmb Modelmentioning

confidence: 99%

“…Based on highresolution observations and a physical model of the jet flow, the presence of velocity shear has been established in a number of low-power jets: those in the radio galaxies 3C 31 (Laing & Bridle 2004), B2 0326+39 and B2 1553+24 (Canvin & Laing 2004), and NGC 315 (Canvin et al 2005). A ''spine-sheath'' shear structure has also been implied for low-power jets based on beaming statistics of FR I and BL Lac objects in the B2 survey (Capetti et al 2002), as well as from polarimetric observations of the jet in M87 (Perlman et al 1999).…”

Section: A Two-zone Model From Velocity Shearmentioning

confidence: 99%

“…If correct, the inferred values of À would constitute the first firm measurement of the velocity of high-power jets (for the velocities of low-power jets, see the modeling by Laing & Bridle 2004;Canvin & Laing 2004;Canvin et al 2005) with profound implications for the analysis of jet energetics and composition. Since the increase of the CMB energy density with redshift would cancel the surface brightness dimming with redshift, beamed IC-CMB X-ray jets at high redshift could be cosmic beacons that outshine their quasars (Schwartz 2002).…”

Section: Introductionmentioning

confidence: 99%

See 1 more Smart Citation

NewChandraObservations of the Jet in 3C 273. I. Softer X‐Ray than Radio Spectra and the X‐Ray Emission Mechanism

Jester

Harris

Marshall

et al. 2006

ApJ

124

167

View full text Add to dashboard Cite

The jet in 3C 273 is a high-power quasar jet with radio, optical, and X-ray emission, whose size and brightness allow a detailed study of the emission processes acting in it. We present deep Chandra observations of this jet and analyze the spectral properties of the jet emission from radio through X-rays. We find that the X-ray spectra are significantly softer than the radio spectra in all regions of the bright part of the jet, except for the first bright ''knot A,'' ruling out a model in which the X-ray emission from the entire jet arises from beamed inverse Compton scattering of cosmic microwave background photons in a single-zone jet flow. Within two-zone jet models, we find that a synchrotron origin for the jet's X-rays requires fewer additional assumptions than an inverse Compton model, especially if velocity shear leads to efficient particle acceleration in jet flows.

show abstract

“…Detailed radio studies and sophisticated modeling of the polarization and total intensity in the radio of several nearby FR I sources (like 3C 31, NGC 315, or 3C 296;Laing & Bridle 2004, Laing et al 2006a do reveal jet radial velocity structures, and indicate that the flatter-spectrum radio regions are indeed often associated with the jet boundary shear layers. Unfortunately, only a few kpc-scale low-power jets, e.g., the one hosted by the radio galaxy Centaurus A, can be resolved at X-ray frequencies by the Chandra instrument.…”

Section: Introductionmentioning

confidence: 99%

Chandra Reveals Twin X-ray Jets in the Powerful FR II Radio Galaxy 3C 353

Kataoka

2008

AIP Conference Proceedings

View full text Add to dashboard Cite

We report X-ray imaging of the powerful FR II radio galaxy 3C 353 using the Chandra X-ray Observatory. 3C 353's two 4 ′′ -wide and 2 ′ -long jets allow us to study in detail the internal structure of the large-scale relativistic outflows at both radio and X-ray photon energies with the sub-arcsecond spatial resolution provided by the VLA and Chandra instruments. In a 90 ks Chandra observation, we have detected X-ray emission from most radio structures in 3C 353, including the nucleus, the jet and the counterjet, the terminal jet regions (hotspots), and one radio lobe. We show that the detection of the X-ray emission associated with the radio knots and counterknots, which is most likely non-thermal in origin, puts several crucial constraints on the X-ray emission mechanisms in powerful large-scale jets of quasars and FR II sources. In particular, we show that this detection is inconsistent with the inverse-Compton model proposed in the literature, and instead implies a synchrotron origin of the X-ray jet photons. We also find that the width of the X-ray counterjet is possibly narrower than that measured in radio bands, that the radio-to-X-ray flux ratio decreases systematically downstream along the jets, and that there are substantial (kpc-scale) offsets between the positions of the X-ray and radio intensity maxima within each knot, whose magnitudes increase away from the nucleus. We discuss all these findings in the wider context of the physics of extragalactic jets, proposing some particular though not definitive solutions or interpretations for each problem. In general, we find that the synchrotron X-ray emission of extragalactic large-scale jets is not only shaped by the global hydrodynamical configuration of the outflows, but is also likely to be very sensitive to the microscopic parameters of the jet plasma. A complete, self-consistent model for the X-ray emission of extragalactic jets still remains elusive.

show abstract

Adiabatic relativistic models for the jets in the radio galaxy 3C 31

Cited by 42 publications

References 24 publications

Magnetic fields in jets: ordered or disordered?

Magnetic fields in jets: ordered or disordered?

NewChandraObservations of the Jet in 3C 273. I. Softer X‐Ray than Radio Spectra and the X‐Ray Emission Mechanism

Chandra Reveals Twin X-ray Jets in the Powerful FR II Radio Galaxy 3C 353

Contact Info

Product

Resources

About