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The impact of disk outflows on the structure of short GRB jets at large scales
High Energy Astrophysical Phenomena · Submitted 18 Jan 2024
abstract compiled · 2026-09-23 · no language-model review
The authors' main claim Our results show that the jet and cocoon structure is shaped by the accretion disk wind that alters the effect of dynamical ejecta and may have an impact on the observed afterglow emission.
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The abstract, sentence by sentence
Short Gamma-Ray Bursts (GRBs) are known to be associated with binary neutron star (NSNS) or black hole-neutron star (BHNS) mergers. The detection of gravitational wave and its associated electromagnetic counterparts GW/GRB 170817A has shown that interactions between relativistic jets and mildly relativistic ejecta influence observed radiation. Previous studies simulated a uniform jet propagating through a homologously expanding wind, however, jets and disk outflows are launched together during accretion, making the interaction more complex. We investigate how the disk wind impacts jet propagation at distances $r\sim 10^8\,-\,10^{11}~$cm. We are using two-dimensional special relativistic hydrodynamical simulations. As initial conditions, we remap the outflows from general relativistic magnetohydrodynamical simulations of BH accretion disks that represent post-merger NSNS or BHNS remnants. We account for wind stratification and r-process nucleosynthesis, which alter the pressure profile from that of an ideal gas in the initial conditions. We found that a) self-consistent wind pressure leads to significant changes in the jet collimation and cocoon expansion; b) the angular structure of thermal and kinetic energy components in the jets, cocoons, and winds differ with respect to simple homologous models; c) the temporal evolution of the structure reveals conversion of thermal to kinetic energy being different for each component in the system (jet, cocoon, and wind); d) dynamical ejecta alters the interaction between jets and disk winds. Our results show that the jet and cocoon structure is shaped by the accretion disk wind that alters the effect of dynamical ejecta and may have an impact on the observed afterglow emission.
background contribution method result interpretation main claim
| # | sentence | role | the authors' own work | states the main conclusion | strength |
|---|---|---|---|---|---|
| s0 | Short Gamma-Ray Bursts (GRBs) are known to be associated with binary neutron star (NSNS) or black hole-neutron star (BHNS) mergers. | background 1.00 | 0.03 | 0.01 | asserted 1.00 |
| s1 | The detection of gravitational wave and its associated electromagnetic counterparts GW/GRB 170817A has shown that interactions between relativistic jets and mildly relativistic ejecta influence observed radiation. | background 1.00 | 0.05 | 0.02 | asserted 1.00 |
| s2 | Previous studies simulated a uniform jet propagating through a homologously expanding wind, however, jets and disk outflows are launched together during accretion, making the interaction more complex. | gap 0.88 | 0.05 | 0.02 | asserted 0.99 |
| s3 | We investigate how the disk wind impacts jet propagation at distances $r\sim 10^8\,-\,10^{11}~$cm. | contribution 1.00 | 0.75 | 0.03 | asserted 0.66 |
| s4 | We are using two-dimensional special relativistic hydrodynamical simulations. | method 1.00 | 0.89 | 0.01 | asserted 0.98 |
| s5 | As initial conditions, we remap the outflows from general relativistic magnetohydrodynamical simulations of BH accretion disks that represent post-merger NSNS or BHNS remnants. | method 0.99 | 0.86 | 0.02 | asserted 0.99 |
| s6 | We account for wind stratification and r-process nucleosynthesis, which alter the pressure profile from that of an ideal gas in the initial conditions. | method 0.97 | 0.85 | 0.03 | asserted 1.00 |
| s7 | We found that a) self-consistent wind pressure leads to significant changes in the jet collimation and cocoon expansion; b) the angular structure of thermal and kinetic energy components in the jets, cocoons, and winds differ with respect to simple homologous models; c) the temporal evolution of the structure reveals conversion of thermal to kinetic energy being different for each component in the system (jet, cocoon, and wind); d) dynamical ejecta alters the interaction between jets and disk winds. | result 1.00 | 0.97 | 0.73 | asserted 1.00 |
| s8 | Our results show that the jet and cocoon structure is shaped by the accretion disk wind that alters the effect of dynamical ejecta and may have an impact on the observed afterglow emission. | interpretation 0.72 | 0.95 | 0.91 | hedged possibility 0.63 |
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The paper
Original abstract
Short Gamma-Ray Bursts (GRBs) are known to be associated with binary neutron star (NSNS) or black hole-neutron star (BHNS) mergers. The detection of gravitational wave and its associated electromagnetic counterparts GW/GRB 170817A has shown that interactions between relativistic jets and mildly relativistic ejecta influence observed radiation. Previous studies simulated a uniform jet propagating through a homologously expanding wind, however, jets and disk outflows are launched together during accretion, making the interaction more complex. We investigate how the disk wind impacts jet propagation at distances $r\sim 10^8\,-\,10^{11}~$cm. We are using two-dimensional special relativistic hydrodynamical simulations. As initial conditions, we remap the outflows from general relativistic magnetohydrodynamical simulations of BH accretion disks that represent post-merger NSNS or BHNS remnants. We account for wind stratification and r-process nucleosynthesis, which alter the pressure profile from that of an ideal gas in the initial conditions. We found that a) self-consistent wind pressure leads to significant changes in the jet collimation and cocoon expansion; b) the angular structure of thermal and kinetic energy components in the jets, cocoons, and winds differ with respect to simple homologous models; c) the temporal evolution of the structure reveals conversion of thermal to kinetic energy being different for each component in the system (jet, cocoon, and wind); d) dynamical ejecta alters the interaction between jets and disk winds. Our results show that the jet and cocoon structure is shaped by the accretion disk wind that alters the effect of dynamical ejecta and may have an impact on the observed afterglow emission.
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How the literature uses it
2 arXiv papers cite this in 2 sentences
Papers citing it · 1 sentence without a confident label
Cites it as background 1 paper
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A number of studies have attempted to constrain GRB jet structure through simulations of jets in both collapsar/massive star and compact object merger ambient environments [ref] .
The Gamma-ray Burst Jet Energy Distribution Suggests A Quasi-universal, Weakly Magnetized Jet Evolving Over Cosmic Time · Jet Structure from High Fidelity Simulations · 0.99
What it cites · 12 sentences without a confident label
Uses data or values from 1 paper
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We assume that this DE has a mass loss rate of $Ṁ=10^-2 M_⊙$ s$^-1$ [ref] .
Jets from neutron-star merger remnants and massive blue kilonovae · The Dynamical Ejecta Implementation · 0.88
Cites as background 3 papers
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The first is to assume as a spherical wind expanding homologously and parametrized by its mass loss rate $Ṁ_wind$ and velocity [ref] .
The propagation of relativistic jets in expanding media · Introduction · 0.93
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In addition to the wind characteristics, the dynamics of weakly magnetized jets has been explored [ref] and the impact of the magnetized environment [ref] .
3D magnetised jet break-out from neutron-star binary merger ejecta: afterglow emission from the jet and the ejecta · Introduction · 0.99
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In the post-merger scenario a broad range of temperatures is present [ref] .
Mergers of double neutron stars with one high-spin component: brighter kilonovae and fallback accretion, weaker gravitational waves · Discussion · 0.90
Discussion
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