An analysis of the proper motions of SS 433 radio jets

Hjellming, R. M.; Johnston, K. J.

doi:10.1086/183571

Cited by 219 publications

(186 citation statements)

References 0 publications

Supporting

Mentioning

165

Contrasting

Unclassified

Order By: Relevance

“…The projection on the sky of the precession cone axes of the SS 433 jets is also overlayed. The radio image shows that the eastern wing of W50 exhibits a corkscrew pattern, which mimics the precession of the arcseconds-scale jets from SS 433 (Dubner et al, 1998, Hjellming & Johnston, 1981. Interestingly, there is a hint of a corkscrew pattern visible in the Chandra image ( Fig.…”

Section: Imagingmentioning

confidence: 73%

A multi-wavelength study of the western lobe of W50 powered by the galactic microquasar SS 433

Moldowan¹,

Safi‐Harb²,

Fuchs³

et al. 2005

Advances in Space Research

View full text Add to dashboard Cite

W50 remains the only supernova remnant (SNR) confirmed to harbor a microquasar: the powerful enigmatic source SS 433. Our past study of this fascinating SNR revealed two X-ray lobes distorting the radio shell as well as non-thermal Xrays at the site of interaction between the SS 433 eastern jet and the eastern lobe of W50. In this paper we present the results of a 75 ksec Chandra ACIS-I observation of the peak of W50-west targeted to 1) determine the nature of the X-ray emission and 2) correlate the X-ray emission with that in the radio and infrared domains. We have confirmed that at the site of interaction between the western jet of SS 433 and dense interstellar gas the X-ray emission is non-thermal in nature. The helical pattern observed in radio is also seen with Chandra . No correlation was found between the infrared and X-ray emission.

show abstract

Section: Imagingmentioning

confidence: 73%

A multi-wavelength study of the western lobe of W50 powered by the galactic microquasar SS 433

Moldowan¹,

Safi‐Harb²,

Fuchs³

et al. 2005

Advances in Space Research

View full text Add to dashboard Cite

show abstract

“…Most prominent examples for this type of model are Hjellming & Johnston (1981) (a kinematic model for SS433 X-ray binary), Raga et al (1993) (an analytical model for the expansion of jets that get ejected with a time-dependent direction), Biro et al (1995) (a 2D numerical simulation based on the analytical model of Raga et al 1993, considering adiabatic and non-adiabatic expansion of the jet), Cliffe et al (1996) (a 3D numerical simulation for precessing stellar jets considering interaction with the surrounding medium), and Stirling et al (2002). Along the lines of Hjellming & Johnston (1981), Gower et al (1982) produced a similar model for radio AGN jets, taking into account projection, relativistic, and cosmological redshift effects. This family of models again does not answer the problem of how the original precession arises, but they do offer a plausible explanation of the evolution of such perturbed jets.…”

Section: Garden Hose Modelsmentioning

confidence: 99%

The kinematics in the pc-scale jets of AGN

Britzen¹,

Kudryavtseva

Witzel³

et al. 2010

A&A

View full text Add to dashboard Cite

Context. BL Lac objects show core-jet structures with features moving outwards along the jet. We present a kinematic analysis of jet component motion in the pc-scale jet of the BL Lac object S5 1803+784, which does not reveal long-term outward motion for most of the components. Aims. S5 1803+784 shows complex kinematic phenomena; understanding these provides new insights into the emission processes in BL Lac objects and possibly into the differences between quasars and BL Lac objects. Methods. The blazar S5 1803+784 has been studied with VLBI at ν = 1.6, 2. 3, 5, 8.4, and 15 GHz between 1993.88 and 2005.68 in 26 observing runs. We (re)analyzed the data and present Gaussian model-fits. We collected the already published kinematic information for this source from the literature and re-identified the components according to the new scenario presented in this paper. Altogether, 94 epochs of observations have been investigated. Results. A careful study of the long-term kinematics reveals a new picture for jet component motion in S5 1803+784. In contrast to previously discussed motion scenarios, we find that the jet structure within 12 mas of the core can most easily be described by the coexistence of several bright jet features that remain on the long-term at roughly constant core separations (in addition to the already known "stationary" jet component ∼1.4 mas) and one faint component moving with an apparent superluminal speed (∼19c, based on 3 epochs). While most of the components maintain long-term roughly constant distances from the core, we observe significant, smooth changes in their position angles. We report on an evolution of the whole jet ridge line with time over the almost 12 years of observations. The width of the jet changes periodically with a period of ∼8−9 years. We find a correlation between changes in the position angle and maxima in the total flux-density light-curves. We present evidence for a geometric origin of the observed phenomena and discuss possible models. Conclusions. We find evidence for a significantly different scenario of jet component motion in S5 1803+784 compared to the generally accepted one of outwardly moving jet components, and conclude that the observed phenomena (evolution of the jet ridge line, roughly constant component core separations but with significant position angle changes) can most easily be explained within a geometric model.

show abstract

“…Stirling et al 2003). On the basis of the assumption that the jet components are ejected from a precessing jet nozzle and move along ballistic paths, we fit the bright knots observed in the jet with a simple precessing model (Hjellming & Johston 1981;Baryshev 1983;An et al 2010).…”

Section: Precessing Jetmentioning

confidence: 99%

Radio structure of the blazar 1156 + 295 with sub-pc resolution

Zhao

Hong

et al. 2011

A&A

View full text Add to dashboard Cite

Aims. 1156+295 is a flat-spectrum quasar that is loud at both radio and γ-ray wavelengths. Previous observations of the source revealed a radio morphology on pc to kpc scales consistent with a helical jet model. We carried out VLBA observations at centimeter and millimeter wavelengths to study the structure of the innermost jet and understand the relation between the helical structure and astrophysical processes in the central engine. Results. A core-jet structure with six jet components is identified in 1156+295. Three jet components are detected for the first time. The apparent transverse velocities of the six jet components derived from proper motion measurements range between 3.6 c and 11.6 c, suggesting that highly relativistic jet plasma moves in the direction close to the line of sight. The overall jet has an oscillating morphology with multiple curvatures on pc scales, which might be indicative of a helical pattern. Models of a helical jet are discussed in the context of both Kelvin-Helmholtz (K-H) instability and jet precession. The K-H instability model is in closer agreement with the observed data. Conclusions. The overall radio structure on scales from sub-pc to kpc appears to be fitted with a hydrodynamic model in the fundamental helical mode of Kelvin-Helmholtz (K-H) instability. This helical mode with an initial characteristic wavelength of λ 0 = 0.2 pc is excited at the base of the jet on the scale of 0.005 pc (or 10 3 R s , the typical size of the broad line region of a supermassive black hole of 4.3 × 10 8 M ). A precessing jet model can also fit the observed jet structure on scales of between 10 pc and 300 pc. However, with the precessing jet model, additional astrophysical processes may be required to explain the bendings of the inner jet structure (1 to 10 pc) and re-collimation of the large-scale jet outflow (>300 pc).

show abstract

An analysis of the proper motions of SS 433 radio jets

Cited by 219 publications

References 0 publications

A multi-wavelength study of the western lobe of W50 powered by the galactic microquasar SS 433

A multi-wavelength study of the western lobe of W50 powered by the galactic microquasar SS 433

The kinematics in the pc-scale jets of AGN

Radio structure of the blazar 1156 + 295 with sub-pc resolution

Contact Info

Product

Resources

About