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
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 / X-rays: binaries / errata, addenda
Our paper Monceau-Baroux 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 d1, while the jet is injected at d0. The factor (and its Lorentz factor γ0, relatively small in the case of SS433) quantifies the squared beam velocity. Given the constant ISM pressure (7.5 × 10-6 g cm-1s-2), the distance d0 = 0.008 pc, and typical density/velocity values, this can quantify the distance d1 where effects caused by the ISM pressure occur. Unfortunately, the estimate d1 ≈ 8.5d0 (i.e. 0.068 pc) we quoted in Eq. (3) used the ISM density for ρ0 (namely ρISM = 8.3 × 10-24 g cm-3), together with a beam speed of vb = 0.26c. A corrected estimate with the actual beam density adopted in our study (ρb = 2.58 × 10-22 g cm-3 at injection) instead gives d1 ≈ 47.6d0, 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 θprec = 20° enters the left-hand side. If we quantify where the beam flow component away from the precession axis (i.e., adopt v0 = vbsin(θprec)) matches the ISM pressure in ram pressure, we obtain d1 ≈ 15.8d0, 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 jet-ISM interaction rather progresses with a decreased head speed of 0.185c due to deceleration (Monceau-Baroux et al. 2014), which further reduces the recollimation distance. Furthermore, the jet propagation itself disturbs and modifies the neighboring density-pressure 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/πvbPISM)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 = 1039 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.
We thank Michael Bowler for pointing out this error, and bringing up relevant references and discussions.
- Eichler, D. 1983, ApJ, 272, 48 [NASA ADS] [CrossRef] (In the text)
- Monceau-Baroux, R., Porth, O., Meliani, Z., & Keppens, R. 2014, A&A, 561, A30 [NASA ADS] [CrossRef] [EDP Sciences] (In the text)
- Monceau-Baroux, R., Porth, O., Meliani, Z., & Keppens, R. 2015, A&A, 574, A143 [NASA ADS] [CrossRef] [EDP Sciences] (In the text)
© ESO, 2017