Dynamics of a supernova envelope in a cloudy interstellar medium

Korolev, Vitaliy; Vasiliev, E. O.; Kovalenko, I. G.; Shchekinov, Yu. A.

doi:10.1134/s1063772915070057

Cited by 27 publications

(19 citation statements)

References 54 publications

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“…However, so small age of W 50's spherical component, obtained in the simulations, contradicts not only to our result, based on a theory for the shock dynamics of SNRs, but also to the simulations on SNRs elsewhere (e.g. Kim & Ostriker 2015;Korolev et al 2015). Goodall et al 's (2011b) simulations invoke the intermittent activity of the jets for the observed shape of the ears.…”

Section: Discussioncontrasting

confidence: 89%

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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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Section: Discussioncontrasting

confidence: 89%

“…In the case of the inhomogeneity, the bubble expands faster, therefore its age for a given radius is smaller, that depends on the volume filling (e.g. Korolev et al 2015, Fig. 4).…”

Section: Physical Conditions Inside the Radio Nebula W 50mentioning

confidence: 99%

Jets of SS 433 on scales of dozens of parsecs

Panferov

2017

A&A

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“…In preliminary calculations we have found that the shape and size of shocked clouds is strongly affected, but the overall evolution of the remnant, for ages early enough that the remnant has not yet gone radiative as a whole, is not substantially changed. Korolev et al (2015) have recently studied the longer term evolution of SNR evo- Figure 12. Evolution of the 0.5 − 7 keV photon luminosity in our simulations.…”

Section: Discussionmentioning

confidence: 99%

Numerical Simulations of Supernova Remnant Evolution in a Cloudy Interstellar Medium

Slavin¹,

Foster²,

Winter³

et al. 2017

ApJ

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The mixed morphology class of supernova remnants has centrally peaked X-ray emission along with a shell-like morphology in radio emission. White & Long proposed that these remnants are evolving in a cloudy medium wherein the clouds are evaporated via thermal conduction once being overrun by the expanding shock. Their analytical model made detailed predictions regarding temperature, density and emission profiles as well as shock evolution. We present numerical hydrodynamical models in 2D and 3D including thermal conduction, testing the White & Long model and presenting results for the evolution and emission from remnants evolving in a cloudy medium. We find that, while certain general results of the White & Long model hold, such as the way the remnants expand and the flattening of the X-ray surface brightness distribution, in detail there are substantial differences. In particular we find that the X-ray luminosity is dominated by emission from shocked cloud gas early on, leading to a bright peak which then declines and flattens as evaporation becomes more important. In addition, the effects of thermal conduction on the intercloud gas, which is not included in the White & Long model, are important and lead to further flattening of the X-ray brightness profile as well as lower X-ray emission temperatures.

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“…It is revealed in numerical simulations that not every such interaction of an impinging shock with clumps stimulates star formation. More often clumps or clouds and their ensembles are destroyed by shockwaves (e.g., Klein et al 1994;Poludnenko et al 2002;Korolev et al 2015;Pittard & Parkin 2016).…”

Section: Introductionmentioning

confidence: 99%

Star formation in shells of colliding multi-SNe bubbles

Vasiliev

Shchekinov

2017

Open Astronomy

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It is believed that when bubbles formed by multiple supernovae explosions interact with one another, they stimulate star formation in overlapping shells. We consider the evolution of a shocked layer formed by the collision of two identical bubbles each of which originated from OB clusters of ∼ 50 members and ∼ 50 pc. The clusters are separated by 200-400 pc. We found that depending on evolutionary status of colliding bubbles the shocked layer can either be destroyed into diffuse lumps, or be fragmented into dense clumps: the former occurs in collisions of young bubbles with continuing supernovae explosions, and the latter occurs in older bubble interactions. We argue that fragmentation efficiency in shells depends on external heating: for a heating rate < ∼ 1.7×10 −24 erg s −1 the number of fragments formed in a collision of two old bubbles reaches several tens at t ∼ 4 Myr, while a heating rate > ∼ 7 × 10 −24 erg s −1 prevents fragmentation. The clumps formed in freely expanding parts of bubbles are gradually destroyed and disappear on t < ∼ 1 Myr, whereas those formed in the overlapping shells survive much longer. Because of this the number of fragments in an isolated bubble begins to decrease after reaching a maximum, while in collision of two old bubbles it fluctuates around 60-70 until longer than t ∼ 5 Myr.

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Dynamics of a supernova envelope in a cloudy interstellar medium

Cited by 27 publications

References 54 publications

Jets of SS 433 on scales of dozens of parsecs

Jets of SS 433 on scales of dozens of parsecs

Numerical Simulations of Supernova Remnant Evolution in a Cloudy Interstellar Medium

Star formation in shells of colliding multi-SNe bubbles

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