The formation of slow-massive-wide jets

Soker, Noam

doi:10.1016/j.newast.2007.11.003

Cited by 10 publications

(23 citation statements)

References 32 publications

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“…This might lead to a high accretion rate that results in very strong jets, that ejected a large fraction of the cooling gas back to large radii. Second, the cooling catastrophe occurred after a hot dense intracluster medium (ICM) was built up in the cluster, such that large quantities of gas could cool, disturb the relativistic jets and form slower, denser and wider jets (Soker 2008). Third, most likely there is a massive BH companion to the central BH of MS 0735 (Pizzolato & Soker 2005b).…”

Section: The Energetic Outburst Of Ms 0735mentioning

confidence: 99%

Explaining the energetic AGN outburst of MS 0735+7421 with massive slow jets

Sternberg

Soker

2009

Monthly Notices of the Royal Astronomical Society

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By conducting axisymmetrical hydrodynamical numerical simulations (2.5 dimensional code) we show that slow, massive, wide jets can reproduce the morphology of the huge X‐ray deficient bubble pair in the cluster of galaxies MS 0735+7421. The total energy of the jets, composed of the energy in the bubble pair and in the shock wave, is constrained by observations conducted by McNamara et al. to be ∼1062 erg. We show that two opposite jets that are active for ∼100 Myr, each with a launching half opening angle of α≃ 70°, an initial velocity of vj∼ 0.1 c and a total mass loss rate of the two jets of , can account for the observed morphology. Rapidly precessing narrow jets can be used instead of wide jets. In our model the cluster suffered from a cooling catastrophe ∼100 Myr ago. Most of the mass that cooled, ∼1010 M⊙, was expelled back to the intracluster medium by the active galactic nuclei activity and is inside the bubbles now, ∼10 per cent formed stars and ∼10 per cent of the cold gas was accreted by the central black hole and was the source of the outburst energy. This type of activity is similar to that expected to occur in galaxy formation.

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Section: The Energetic Outburst Of Ms 0735mentioning

confidence: 99%

Explaining the energetic AGN outburst of MS 0735+7421 with massive slow jets

Sternberg

Soker

2009

Monthly Notices of the Royal Astronomical Society

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“…This mechanism where the negative feedback is based on the jets’ non‐penetrating condition is termed the penetrating jet feedback mechanism. It was suggested to operate in forming SMW jets (Soker 2008) and to regulate the growth of the super massive BH during galaxy formation (Soker 2009; Soker & Meiron 2011). Namely, we suggest that NSs (or BHs) at the centre of CCSNe shut off their own growth and expel the rest of the mass available for accretion by the same mechanism, via jets, that super massive BHs shut off their own growth, as well as that of their host bulge, in young galaxies.…”

Section: Discussionmentioning

confidence: 99%

“…In Paper I the same mechanism that was used to explain the formation of SMW jets in other astrophysical systems was proposed to operate in CCSNe. This mechanism is the penetrating jet feedback mechanism , that was applied to the growth of the super massive black hole (BH) during galaxy formation (Soker 2009; Soker & Meiron 2011), and to stellar environments (Soker 2008). When the jets penetrate through the ambient medium to large distances, they do not heat and do not expel the gas, and accretion on to the central region might continue.…”

Section: Introductionmentioning

confidence: 99%

Exploding core collapse supernovae with jittering jets

Papish¹,

Soker²

2011

Monthly Notices of the Royal Astronomical Society

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We argue that jittering jets, i.e. jets that have their launching direction rapidly change, launched by the newly formed neutron star in a core‐collapse supernova can explode the star. We show that under a wide range of parameters the fast narrow jets deposit their energy inside the star via shock waves, and form two hot bubbles, that eventually merge, accelerate the rest of the star and lead to the explosion. To prevent the jets from penetrating through the collapsing stellar core and escape with their energy, instead of forming the hot bubbles, the jets should be prevented from drilling a hole through the star. This condition can be met if the jets’ axis rapidly changes its direction. This process of depositing jets’ energy into the ambient medium is termed the penetrating jet feedback mechanism. The feedback exists in that the neutron star (or a black hole) at the centre of the core‐collapse supernova shuts off its own growth by exploding the star. The jets deposit their energy at a distance of ∼1000 km from the centre and expel the mass above that radius. In our model, the material near the stalled shock at several hundreds kilometers from the centre is not expelled, but it is rather accreted and feed the accretion disc that blows the jets. The neutrinos might influence the accretion flow, but in the proposed model their role in exploding the star is small.

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“…For more detail on the numerical code and the properties of the jets, see Sternberg & Soker (2008b). The motivation for using slow‐massive‐wide jets, from both theoretical and observational arguments, is discussed in some length in previous papers (Sternberg et al 2007; Soker 2008).…”

Section: Numerical Methods and Setupmentioning

confidence: 99%

Sound waves excitation by jet-inflated bubbles in clusters of galaxies

Sternberg

Soker

2009

Monthly Notices of the Royal Astronomical Society

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We show that repeated sound waves in the intracluster medium (ICM) can be excited by a single inflation episode of an opposite bubble pair. To reproduce this behaviour in numerical simulations, the bubbles should be inflated by jets, rather than being injected artificially as already full‐blown bubbles. The multiple sound waves are excited by the motion of the bubble–ICM boundary that is caused by vortices inside the inflated bubbles and the backflow (‘cocoon’) of the ICM around the bubble. These sound waves form a structure that can account for the ripples observed in the Perseus cooling flow cluster. We inflate the bubbles using slow massive jets either with a very wide opening angle or that are narrow and precessing. The wide jets (or collimated fast winds) are slow in the sense that they are highly subrelativistic, vj∼ 0.01c– 0.1c, and they are massive in the sense that the pair of bubbles carries back to the ICM a large fraction of the cooling mass, i.e. ∼1–50 M⊙ yr−1. We use a two‐dimensional axisymmetric (referred to as 2.5D) hydrodynamical numerical code (vh‐1).

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The formation of slow-massive-wide jets

Cited by 10 publications

References 32 publications

Explaining the energetic AGN outburst of MS 0735+7421 with massive slow jets

Explaining the energetic AGN outburst of MS 0735+7421 with massive slow jets

Exploding core collapse supernovae with jittering jets

Sound waves excitation by jet-inflated bubbles in clusters of galaxies

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