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Collimation and confinement of magnetic jets by external media
High Energy Astrophysical Phenomena · Submitted 24 Sep 2012
abstract compiled · 2026-09-23 · no language-model review
The authors' main claim We apply the model to jet breakout in long GRBs, and show that the jet is highly collimated inside the envelope of the progenitor star, and is likely to remain confined well after breakout.
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The abstract, sentence by sentence
We study the collimation of a highly magnetized jet by a surrounding cocoon that forms as a result of the interaction of the jet with the external medium. We show that in regions where the jet is well confined by the cocoon, current-driven instabilities should develop over timescales shorter than the expansion time of the jet's head. We speculate that these instabilities would give rise to complete magnetic field destruction, whereby the jet undergoes a transition from high-to-low sigma above the collimation zone. Using this assumption, we construct a self-consistent model for the evolution of the jet-cocoon system in an ambient medium of arbitrary density profile. We apply the model to jet breakout in long GRBs, and show that the jet is highly collimated inside the envelope of the progenitor star, and is likely to remain confined well after breakout. We speculate that this strong confinement may provide a channel for magnetic field conversion in GRB outflows, whereby the hot, low-sigma jet section thereby produced is the source of the photospheric emission observed in many bursts.
background contribution method result interpretation main claim
| # | sentence | role | the authors' own work | states the main conclusion | strength |
|---|---|---|---|---|---|
| s0 | We study the collimation of a highly magnetized jet by a surrounding cocoon that forms as a result of the interaction of the jet with the external medium. | contribution 0.92 | 0.74 | 0.08 | asserted 0.91 |
| s1 | We show that in regions where the jet is well confined by the cocoon, current-driven instabilities should develop over timescales shorter than the expansion time of the jet's head. | result 0.98 | 0.84 | 0.18 | asserted 0.95 |
| s2 | We speculate that these instabilities would give rise to complete magnetic field destruction, whereby the jet undergoes a transition from high-to-low sigma above the collimation zone. | interpretation 0.98 | 0.12 | 0.17 | speculative 1.00 |
| s3 | Using this assumption, we construct a self-consistent model for the evolution of the jet-cocoon system in an ambient medium of arbitrary density profile. | method 0.95 | 0.94 | 0.06 | asserted 0.98 |
| s4 | We apply the model to jet breakout in long GRBs, and show that the jet is highly collimated inside the envelope of the progenitor star, and is likely to remain confined well after breakout. | result 0.93 | 0.94 | 0.30 | asserted 0.69 |
| s5 | We speculate that this strong confinement may provide a channel for magnetic field conversion in GRB outflows, whereby the hot, low-sigma jet section thereby produced is the source of the photospheric emission observed in many bursts. | interpretation 1.00 | 0.25 | 0.24 | speculative 0.99 |
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The paper
Original abstract
We study the collimation of a highly magnetized jet by a surrounding cocoon that forms as a result of the interaction of the jet with the external medium. We show that in regions where the jet is well confined by the cocoon, current-driven instabilities should develop over timescales shorter than the expansion time of the jet's head. We speculate that these instabilities would give rise to complete magnetic field destruction, whereby the jet undergoes a transition from high-to-low sigma above the collimation zone. Using this assumption, we construct a self-consistent model for the evolution of the jet-cocoon system in an ambient medium of arbitrary density profile. We apply the model to jet breakout in long GRBs, and show that the jet is highly collimated inside the envelope of the progenitor star, and is likely to remain confined well after breakout. We speculate that this strong confinement may provide a channel for magnetic field conversion in GRB outflows, whereby the hot, low-sigma jet section thereby produced is the source of the photospheric emission observed in many bursts.
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References
How the literature uses it
6 arXiv papers cite this in 7 sentences
Papers citing it · 5 sentences without a confident label
Cites it as background 2 papers
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The propagation of a jet+cocoon through an ambient medium has been investigated in different setups (e.g., static or expanding medium, magnetized or hydrodynamic jets) by several authors [ref] .
Cocoon shock breakout emission from binary neutron star mergers · Jet and cocoon propagation within the ejecta · 1.00
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In general, jet collimation is affected by many physical parameters, such as the black hole spin [ref] , magnetic field structure and strength [ref] , disk wind pressure [ref] , and the density of the external medium [ref] .
Three-dimensional GRMHD simulations of jet formation and propagation in self-gravitating collapsing stars · Jet opening angle · 0.84
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