When microquasar jets and supernova collide: hydrodynamically simulating the SS 433-W 50 interaction

Goodall, Paul T.; Alouani-Bibi, F.; Blundell, Katherine M.

doi:10.1111/j.1365-2966.2011.18388.x

Cited by 57 publications

(89 citation statements)

References 47 publications

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“…In particular, Goodall et al (2011b) resume that in the case of a permanency the SS 433 jet should decelerate only at the terminal shock, i.e. in the ear.…”

Section: Introductionmentioning

confidence: 92%

Jets of SS 433 on scales of dozens of parsecs

Panferov

2017

A&A

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The radio nebula W 50 harbours the relativistic binary system SS 433, which is a source of the powerful wind and jets. The origin of W 50 is wrapped in the interplay of the wind, supernova remnant and jets. The evolution of the jets on the scales of the nebula is a Rosetta stone for its origin.To disentangle the roles of these components, we study physical conditions of the jets propagation inside W 50, and determine deceleration of the jets.The morphology and parameters of the interior of W 50 are analyzed using the available observations of the eastern X-ray lobe, which traces the jet.In order to estimate deceleration of this jet, we devised a simplistic model of the viscous interaction, via turbulence, of a jet with the ambient medium, which would fit mass entrainment from the ambient medium into the jets of the radio galaxy 3C 31, the well studied case of continuously decelerating jets.X-ray observations suggest that the eastern jet persists through W 50 as hollow one, and is recollimated to the opening ∼ 30• . From the thermal emission of the eastern X-ray lobe, we determine a pressure of P ∼ 3 · 10 −11 erg/cm 3 inside W 50. In the frame of a theory of the dynamics of radiative supernova remnants and stellar wind bubbles, this pressure in combination with other known parameters restricts W 50's origin to a supernova happened ∼ 100 000 yr ago. Also, this pressure in our entrainment model gives a deceleration of the jet by ∼ 60% in the bounds of W 50's spherical component, of radius ∼ 40 pc. In this case, the age of the jet should be 27 000 yr so as to satisfy the sphericity of W 50.The entrainment model comes to the viscous stress in a jet of a form σ = αP, where the viscosity parameter α is predefined by the model.

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“…In particular, Goodall et al (2011b) resume that in the case of a permanency the SS 433 jet should decelerate only at the terminal shock, i.e. in the ear.…”

Section: Introductionmentioning

confidence: 92%

Jets of SS 433 on scales of dozens of parsecs

Panferov

2017

A&A

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“…According to Goodall et al (2011), the asymmetry of W50 is due to the exponential density profile of the Milky Way disc. We can similarly explain the asymmetry in the extent of the lobes of the SNR in IC 2574 by the density gradient in the wall of the SGS.…”

Section: Hii-complexes With Estimates Of the Upper Limit Of The Expanmentioning

confidence: 99%

“…We can speculate that the Hα morphology of the SNR in IC 2574 considered here (a central shell and two symmetrical 'lobes' north and south of it) resembles very much the structure of the well-known Galactic SNR W50 with two symmetric eastern and western 'lobes' due to jets emerging from the central SS 433 microquasar (see Goodall, Alouani-Bibi & Blundell 2011, for a recent analysis).…”

Section: Hii-complexes With Estimates Of the Upper Limit Of The Expanmentioning

confidence: 99%

The supergiant shell with triggered star formation in the dwarf irregular galaxy IC 2574: neutral and ionized gas kinematics

Egorov¹,

Lozinskaya²,

Моисеев³

et al. 2014

Monthly Notices of the Royal Astronomical Society

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We analyse the ionized gas kinematics in the star formation regions of the supergiant shell (SGS) of the IC 2574 galaxy using observations with the Fabry-Perot interferometer at the 6-m telescope of SAO RAS; the data of the THINGS survey are used to analyze the neutral gas kinematics in the area. We perform the 'derotation' of the Hα and H i data cubes and show its efficiency in kinematics analysis. We confirm the SGS expansion velocity 25 km s −1 obtained by Walter & Brinks (1999) and conclude that the SGS is located at the far side of the galactic disc plane. We determine the expansion velocities, kinematic ages, and the required mechanical energy input rates for four star formation complexes in the walls of the SGS; for the remaining ones we give the limiting values of the above parameters. A comparison with the age and energy input of the complexes' stellar population shows that sufficient energy is fed to all H ii regions except one. We discuss in detail the possible nature of this region and that of another one, which was believed to be an SNR according to radio observations. We measured the expansion velocity of the latter and confirm its identification as an old SNR. Our observations allowed us to identify a faint diffuse Hα emission inside the SGS which was never observed before.

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“…Goodall et al 2011). These binaries have dual, parsec-scale termination shocks of the bipolar jets referred to as "ears" for SS 433 (e.g.…”

Section: The Black Hole Jetmentioning

confidence: 99%

Shell-shocked: the interstellar medium near Cygnus X-1

Sell

Heinz

Richards

et al. 2014

Monthly Notices of the Royal Astronomical Society

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We conduct a detailed case-study of the interstellar shell near the high-mass X-ray binary, Cygnus X-1. We present new WIYN optical spectroscopic and Chandra X-ray observations of this region, which we compare with detailed MAPPINGS III shock models, to investigate the outflow powering the shell. Our analysis places improved, physically motivated constraints on the nature of the shockwave and the interstellar medium (ISM) it is plowing through. We find that the shock is traveling at less than a few hundred km s −1 through a low-density ISM (< 5 cm −3 ). We calculate a robust, 3σ upper limit to the total, time-averaged power needed to drive the shockwave and inflate the bubble, < 2×10 38 erg s −1 . We then review possible origins of the shockwave. We find that a supernova origin to the shockwave is unlikely and that the black hole jet and/or O-star wind can both be central drivers of the shockwave. We conclude that the source of the Cygnus X-1 shockwave is far from solved.

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When microquasar jets and supernova collide: hydrodynamically simulating the SS 433-W 50 interaction

Cited by 57 publications

References 47 publications

Jets of SS 433 on scales of dozens of parsecs

Jets of SS 433 on scales of dozens of parsecs

The supergiant shell with triggered star formation in the dwarf irregular galaxy IC 2574: neutral and ionized gas kinematics

Shell-shocked: the interstellar medium near Cygnus X-1

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