Symmetry in the Changing Jets of SS 433 and Its True Distance from Us

Blundell, Katherine M.; Bowler, M.G.

doi:10.1086/426542

Cited by 124 publications

(168 citation statements)

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“…W50 is an extended SNR located at about 5.5 kpc (Blundell & Bowler 2004;Lockman et al 2007). It consists of a central component with a diameter of about 1 • and two "ears" extended to the northwest and southeast (see Fig.…”

Section: G397−20 (W50)mentioning

confidence: 99%

A Sino-Germanλ6 cm polarization survey of the Galactic plane

Gao

Han

Reich

et al. 2011

A&A

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Context.Observations of large supernova remnants (SNRs) at high frequencies are rare, but provide valuable information about their physical properties. Aims. The total intensity and polarization properties of 16 large SNRs in the Galactic plane are investigated based on observations of the Urumqi λ6 cm polarization survey of the Galactic plane with an angular resolution of 9. 5. Methods. We extracted total intensity and linear polarization maps of large SNRs from the Urumqi λ6 cm survey, obtained their integrated flux densities, and derived the radio spectra by using these flux densities together with previously published flux densities at various frequencies. In particular, Effelsberg λ11 cm and λ21 cm survey data were used to calculate integrated flux densities. The λ6 cm polarization data also delineate the magnetic field structures of the SNRs. Results. We present the first total intensity maps at λ6 cm for SNRs G106.3+2.7, G114.3+0.3, G116.5+1.1, G166.0+4.3 (VRO 42.05.01), G205.5+0.5 (Monoceros Nebula), and G206.9+2.3 (PKS 0646+06) and the first polarization measurements at λ6 cm for SNRs G82.2+5.3 (W63), G106.3+2.7, G114.3+0.3, G116.5+1.1, G166.0+4.3 (VRO 42.05.01), G205.5+0.5 (Monoceros Nebula), and G206.9+2.3 (PKS 0646+06). Most of the newly derived integrated radio spectra are consistent with previous results. The new flux densities obtained from the Urumqi λ6 cm, Effelsberg λ11 cm and λ21 cm surveys are crucial to determine the spectra of SNR G65.1+0.6, G69.0+2.7 (CTB 80), G93.7−0.2, and G114.3+0.3. We find that G192.8−1.1 (PKS 0607+17) consists of background sources, H ii regions, and extended diffuse emission of thermal nature, and conclude that G192.8−1.1 is not a SNR.

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Section: G397−20 (W50)mentioning

confidence: 99%

A Sino-Germanλ6 cm polarization survey of the Galactic plane

Gao

Han

Reich

et al. 2011

A&A

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“…jets on a scale of several arcseconds) is larger than the distance determined by the kinematics of the inner jets (i.e. jets on a sub-arcsecond scale): 5.5 ± 0.2 kpc (Hjellming & Johnston, 1981;Blundell & Bowler, 2004) from images unresolved in time of the extended jets vs. the estimates 4.9 ± 0.2 kpc (Spencer, 1984), 4.85 ± 0.2 kpc (Vermeulen et al, 1993) and 4.61 ± 0.35 kpc (Stirling et al, 2002) from proper motion of radio knots in the inner jets, and 5.0 ± 0.3 kpc (Fejes, 1986) and 5.0 ± 0.5 kpc (Romney et al, 1987) from images unresolved in time of the inner jets. This dichotomy might be explained by the fact that an a priori assumption of constancy of the jet velocity in kinematic simulations of really decelerating jets leads to an overestimate of the distance to SS 433, D, so that the model jet matches the observed angular jet size, which is proportional in the first approximation to the ratio v j /D.…”

Section: Introductionmentioning

confidence: 98%

“…Though the radio jets at their origin are intimately connected with the optical jets, which are believed to be ballistic (Kopylov et al, 1987), their behaviour differs slightly: the radio jets deviate from the kinematics of the optical jets by more than 10% (e.g. Blundell & Bowler, 2004;Schillemat et al, 2004;Roberts et al, 2008); the radio clouds can be found far away from the jets (e.g. Spencer, 1984;Romney et al, 1987); the radio jets appear to be more continuous (e.g.…”

Section: Introductionmentioning

confidence: 99%

Simulation of kinematics of SS 433 radio jets that interact with the ambient medium

Panferov

2014

A&A

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Context. The mildly relativistic jets of SS 433 are believed to inflate the surrounding supernova remnant W 50, possibly depositing more than 99% of their kinetic energy in the remnant expansion. Where and how this transformation of the energy occurs is as yet unknown. We can learn from this that the jets decelerate and that this deceleration is non-dissipative. Aims. We uncover the deviation of the arcsecond-scale precessing radio jets of SS 433 from the ballistic locus described by the kinematic model as a signature of the dynamics issuing from the interaction of the jets with the ambient medium. Methods. To do this, we simulated the kinematics of these jets, taking into account the ram pressure on the jets, which we estimated from the profile of brightness of synchrotron radiation along the radio jets, assuming pressure balance in the jets. Results. We found that to fit an observable locus in all scales the radio jets need to be decelerated and twisted in addition to the precession torsion, mostly within the first one-fifth of the precession period, and subsequently they extend in a way that imitates ballistic jets. This jet kinematics implies a smaller distance to SS 433 than the currently accepted 5.5 kpc. The physical parameters of the jet model, which links jets dynamics with radiation, are physically reliable and characteristic for the SS 433 jets. The model proposes that beyond the radio-brightening zone, the jet clouds expand because they are in pressure balance with the intercloud medium, and heat up with distance according to the law T = 2 × 10 4 (r/10 15 cm) 1.5 K. Conclusions. This model naturally explains and agrees with, the observed properties of the radio jets: a) the shock-pressed morphology; b) the brightness profile; c) the ∼10% deflections of the jet kinematics from the standard kinematic model -a magnitude of the jet speed decrement in our simulation; d) the precession-phase deviations from the standard kinematic model predictions; e) the dichotomy of the distances to the object, 4.8 kpc vs. 5.5 kpc, which are determined on the basis of the jet kinematics on scales of sub-arcsecond and several arcseconds, respectively; and f) the reheating on arcsecond scales.

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“…The distance of SS 433 has also remained uncertain for a long time. From complete observations of the radio emitting materials ejected in the relativistic jets and after taking the kinematic model into account, Blundell & Bowler (2004) eventually determined this distance as d = 5.5 ± 0.2 kpc.…”

Section: Introductionmentioning

confidence: 99%

SS 433: a phenomenon imitating a Wolf-Rayet star

Fuchs

Miramond

Ábrahám

2006

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We present mid-infrared (2-12 µm) spectra of the microquasar SS 433 obtained with the Infrared Space Observatory (spectroscopic mode of ISOPHOT and ISOCAM). We compare them to the spectra of four Wolf-Rayet stars: WR 78, WR 134, WR 136, and WR 147 in the same wavelength range. The mid-infrared spectrum of SS 433 mainly shows H i and He i emission lines and is very similar to the spectrum of WR 147, a WN8(h)+B0.5V binary. The 2-12 µm continuum emission of SS 433 corresponds to optically thin and partially optically thick free-free emission, from which we calculate a mass loss rate of 2−3 × 10 −4 M yr −1 if the wind is homogeneous and a third of these values if it is clumped. This is consistent with a strong stellar wind from a WN star. However, following recent studies concluding that the mass donor star of SS 433 is not a Wolf-Rayet star, we propose that this strong wind out flows from a geometrically thick envelope of material that surrounds the compact object like a stellar atmosphere, imitating the Wolf-Rayet phenomenon. This wind could also wrap the mass donor star, and at larger distances (∼40 AU), it might form a dust envelope from which the thermal emission, detected with ISOPHOT at 25 µm and 60 µm, would originate. This wind also probably feeds the material that is ejected in the orbital plane of the binary system and that forms the equatorial outflow detected in radio at distances > 100 AU.

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Symmetry in the Changing Jets of SS 433 and Its True Distance from Us

Cited by 124 publications

References 12 publications

A Sino-Germanλ6 cm polarization survey of the Galactic plane

A Sino-Germanλ6 cm polarization survey of the Galactic plane

Simulation of kinematics of SS 433 radio jets that interact with the ambient medium

SS 433: a phenomenon imitating a Wolf-Rayet star

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