Issue 
A&A
Volume 607, November 2017



Article Number  C4  
Number of page(s)  1  
Section  Astrophysical processes  
DOI  https://doi.org/10.1051/00046361/201425015e  
Published online  20 November 2017 
The SS433 jet from subparsec to parsec scales (Corrigendum)
^{1} Centre for mathematical Plasma Astrophysics, Department of Mathematics, KU Leuven, Celestijnenlaan 200B, 3001 Heverlee, Belgium
email: remi.monceaubaroux@gmail.com
^{2} Institute for Theoretical Physics, Frankfurt am Main, 60438 Germany
^{3} LUTh, Observatoire de Paris, France
Key words: hydrodynamics / relativistic processes / ISM: jets and outflows / Xrays: binaries / errata, addenda
Our paper MonceauBaroux et al. (2015) presented numerical simulations of the precessing SS433 jet up to parsec scales, and its main finding was a dynamical recollimation effect: the jet transits from a winding helix to a more hollow straight jet. We argued that this transition occurred at 0.068 parsec, and gave a physical argument based on ram pressure that balances the pressure of the interstellar medium (ISM). This writes as (our Eq. (2)), where the is intended to estimate the density decrease in the jet beam at a distance d_{1}, while the jet is injected at d_{0}. The factor (and its Lorentz factor γ_{0}, relatively small in the case of SS433) quantifies the squared beam velocity. Given the constant ISM pressure (7.5 × 10^{6} g cm^{1}s^{2}), the distance d_{0} = 0.008 pc, and typical density/velocity values, this can quantify the distance d_{1} where effects caused by the ISM pressure occur. Unfortunately, the estimate d_{1} ≈ 8.5d_{0} (i.e. 0.068 pc) we quoted in Eq. (3) used the ISM density for ρ_{0} (namely ρ_{ISM} = 8.3 × 10^{24} g cm^{3}), together with a beam speed of v_{b} = 0.26c. A corrected estimate with the actual beam density adopted in our study (ρ_{b} = 2.58 × 10^{22} g cm^{3} at injection) instead gives d_{1} ≈ 47.6d_{0}, which is factor of 5.6 larger. This value clearly overestimates the distance where recollimation was found to occur (see Figs. 4, 6, or 8 in our paper). An improved estimate can be obtained by acknowledging that the ram pressure acts directional, such that a projection using the fixed precession angle θ_{prec} = 20° enters the lefthand side. If we quantify where the beam flow component away from the precession axis (i.e., adopt v_{0} = v_{b}sin(θ_{prec})) matches the ISM pressure in ram pressure, we obtain d_{1} ≈ 15.8d_{0}, or a distance of 0.126 parsec. This is in better agreement with the observed recollimation. Deviations from this simple estimate
can be understood from the fact that the full 3D jetISM interaction rather progresses with a decreased head speed of 0.185c due to deceleration (MonceauBaroux et al. 2014), which further reduces the recollimation distance. Furthermore, the jet propagation itself disturbs and modifies the neighboring densitypressure ISM conditions, and may in particular modify the pressure distribution interior to the helical jet path. This will occur on a timescale associated with the jet thermal expansion toward the axis, and this effect can similarly lower the obtained distance estimate. We further note that earlier models (Eichler 1983) predicted a complete refocusing of a hollow, conical, axisymmetric jet (with zero pressure within the hollow cone) over a distance estimated as 3(L/πv_{b}P_{ISM})^{1/2}, with L the jet power. This model balances the pressure on the jet with the centrifugal force felt by a jet parcel along its curved trajectory in the plane containing the jet axis. As the SS433 kinetic luminosity L = 10^{39} erg s^{1}, this estimate leads to 0.07 pc, implying that deflection effects would occur at half this distance, or at 0.035 pc. Clearly, this underestimates where our simulations find the deflection. This highlights the role of accounting for the full 3D helical nature of the jet flow, and for the finite pressure effects in the jet surroundings.
Acknowledgments
We thank Michael Bowler for pointing out this error, and bringing up relevant references and discussions.
References
 Eichler, D. 1983, ApJ, 272, 48 [NASA ADS] [CrossRef] [Google Scholar]
 MonceauBaroux, R., Porth, O., Meliani, Z., & Keppens, R. 2014, A&A, 561, A30 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
 MonceauBaroux, R., Porth, O., Meliani, Z., & Keppens, R. 2015, A&A, 574, A143 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
© ESO, 2017
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