Relativistic outflows from remnants of compact object mergers and their viability for short gamma-ray bursts

E. Mueller (1) ((1) Max--Planck--Institut fuer Astrophysik); H.-T. Janka (1); M.A. Aloy (1)

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Relativistic outflows from remnants of compact object mergers and their viability for short gamma-ray bursts

M.A. Aloy (1), H.-T. Janka (1), E. Mueller (1) ((1) Max--Planck--Institut fuer Astrophysik)

Astrophysics · Submitted 16 Aug 2004

abstract compiled · 2026-09-23 · no language-model review

The authors' main claim Our models confirm the viability of post-merger BH-torus systems as engines of short, hard GRBs and can explain the durations of all observed short GRBs, because different propagation velocities of the front and rear ends lead to a radial stretching of the ultrarelativistic fireball before transparency is reached.

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arXiv IDastro-ph/0408291 (version 2)

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CitationE. Mueller (1) ((1) Max--Planck--Institut fuer Astrophysik), H.-T. Janka (1), M.A. Aloy (1). "Relativistic outflows from remnants of compact object mergers and their viability for short gamma-ray bursts." arXiv:astro-ph/0408291 (2004). https://pith.science/paper/RNZVBCJ3

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What the abstract itself states, as probabilities: claims first 0.94 · states limitation 0.35 · human participants 0.01 · controlled comparison 0.02 · randomized assignment 0.01 · states quantitative result 0.98 · compares with prior results 0.09 · mentions code or data availability 0.02.

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We present the first general relativistic hydrodynamic models of the launch and evolution of relativistic jets and winds, driven by thermal energy deposition, possibly due to neutrino-antineutrino annihilation, in the close vicinity of black hole-accretion torus systems. The latter are considered to be the remnants of compact object mergers. Our two-dimensional simulations establish the link between such mergers and future observations of short gamma-ray bursts (GRBs) by the SWIFT satellite. They show that ultrarelativistic outflow with maximum terminal Lorentz factors (Gamma) around 1000 develops for polar energy deposition rates above some 1e48 erg/s per steradian, provided the merger environment has a sufficiently low baryon density. Due to the collimation by the dense accretion torus the typical semi-opening angles of the Gamma > 100 cone are 5-10 degrees, corresponding to about 0.4-1.5% of the hemisphere and apparent isotropized energies (kinetic plus internal) up to ~1e51 erg. 10-30% of the deposited energy are transferred to the outflow with Gamma > 100. Our models confirm the viability of post-merger BH-torus systems as engines of short, hard GRBs and can explain the durations of all observed short GRBs, because different propagation velocities of the front and rear ends lead to a radial stretching of the ultrarelativistic fireball before transparency is reached. The ultrarelativistic flow reveals a highly non-uniform structure with Lorentz factor variations up to factors of a few, caused by the action of Kelvin-Helmholtz instabilities that originate at the fireball-torus interface (abbreviated).

background contribution method result interpretation main claim

What the classifier reports for each sentence. The number is the probability it gave the label.
#	sentence	role	the authors' own work	states the main conclusion	strength
s0	We present the first general relativistic hydrodynamic models of the launch and evolution of relativistic jets and winds, driven by thermal energy deposition, possibly due to neutrino-antineutrino annihilation, in the close vicinity of black hole-accretion torus systems.	contribution 0.95	0.95	0.06	asserted 0.55
s1	The latter are considered to be the remnants of compact object mergers.	background 0.99	0.07	0.03	asserted 0.60
s2	Our two-dimensional simulations establish the link between such mergers and future observations of short gamma-ray bursts (GRBs) by the SWIFT satellite.	contribution 0.43	0.88	0.19	asserted 1.00
s3	They show that ultrarelativistic outflow with maximum terminal Lorentz factors (Gamma) around 1000 develops for polar energy deposition rates above some 1e48 erg/s per steradian, provided the merger environment has a sufficiently low baryon density.	result 1.00	0.93	0.16	asserted 0.98
s4	Due to the collimation by the dense accretion torus the typical semi-opening angles of the Gamma > 100 cone are 5-10 degrees, corresponding to about 0.4-1.5% of the hemisphere and apparent isotropized energies (kinetic plus internal) up to ~1e51 erg. 10-30% of the deposited energy are transferred to the outflow with Gamma > 100.	result 1.00	0.93	0.08	asserted 1.00
s5	Our models confirm the viability of post-merger BH-torus systems as engines of short, hard GRBs and can explain the durations of all observed short GRBs, because different propagation velocities of the front and rear ends lead to a radial stretching of the ultrarelativistic fireball before transparency is reached.	interpretation 0.94	0.90	0.79	asserted 1.00
s6	The ultrarelativistic flow reveals a highly non-uniform structure with Lorentz factor variations up to factors of a few, caused by the action of Kelvin-Helmholtz instabilities that originate at the fireball-torus interface (abbreviated).	result 1.00	0.91	0.05	asserted 1.00

What kind of paper the classifier reports this is: simulation study 1.00 · evidence from simulation or computation 1.00.

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arXiv listing abstract v2

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full text
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Original abstract

We present the first general relativistic hydrodynamic models of the launch and evolution of relativistic jets and winds, driven by thermal energy deposition, possibly due to neutrino-antineutrino annihilation, in the close vicinity of black hole-accretion torus systems. The latter are considered to be the remnants of compact object mergers. Our two-dimensional simulations establish the link between such mergers and future observations of short gamma-ray bursts (GRBs) by the SWIFT satellite. They show that ultrarelativistic outflow with maximum terminal Lorentz factors (Gamma) around 1000 develops for polar energy deposition rates above some 1e48 erg/s per steradian, provided the merger environment has a sufficiently low baryon density. Due to the collimation by the dense accretion torus the typical semi-opening angles of the Gamma > 100 cone are 5-10 degrees, corresponding to about 0.4-1.5% of the hemisphere and apparent isotropized energies (kinetic plus internal) up to ~1e51 erg. 10-30% of the deposited energy are transferred to the outflow with Gamma > 100. Our models confirm the viability of post-merger BH-torus systems as engines of short, hard GRBs and can explain the durations of all observed short GRBs, because different propagation velocities of the front and rear ends lead to a radial stretching of the ultrarelativistic fireball before transparency is reached. The ultrarelativistic flow reveals a highly non-uniform structure with Lorentz factor variations up to factors of a few, caused by the action of Kelvin-Helmholtz instabilities that originate at the fireball-torus interface (abbreviated).

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References

Forward citations

Cited by 6 Pith papers

Reviewed papers in the Pith corpus that reference this work. Sorted by Pith novelty score. Full citation record

The (missing) gamma-ray counterparts to EP events
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A systematic search for gamma-ray counterparts to 72 Einstein Probe fast X-ray transients reveals that 68% lack detectable gamma-ray emission, with upper limits consistent with low-energy, low-luminosity gamma-ray bursts.
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An ANN emulator of a kinetic SSC afterglow code enables MCMC inference on GRB 190114C, yielding E_k,iso ~ 7.2e54 erg, Gamma ~ 575, n ~ 0.1 cm^-3, while flagging that the constant-density ISM fails at late times.
Inferring Neutron Star Nuclear Properties from Gravitational-Wave and Gamma-Ray Burst Observations
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By matching LIGO-Virgo-KAGRA merger rates to gamma-ray burst rates, the authors infer that the dividing mass between short and long bursts is about 1.36 times the maximum neutron star mass.
Late time afterglow observations reveal a collimated relativistic jet in the ejecta of the binary neutron star merger GW170817
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A structured jet with a fast core and slower wings, viewed about 33 degrees off-axis, fits the multi-wavelength afterglow of GW170817 and implies binary neutron star mergers produce short gamma-ray bursts.
Neutrino pair annihilation driven jets from black-hole torus systems
astro-ph.HE 2025-06 conditional novelty 5.0 of 10

Neutrino pair annihilation in black hole-torus systems launches relativistic fireballs with isotropic energies up to about 10^51 erg and durations around 0.1 s, which can account for faint short GRBs and GRB precursors.

Show 1 more citing papers

Short-Hard Gamma-Ray Bursts
astro-ph 2007-01 accept novelty 4.0 of 10

Short gamma-ray bursts are a distinct population from long bursts, most likely powered by compact binary mergers, and their afterglows imply low-density environments and modest beaming.

How the literature uses it

12 arXiv papers cite this in 26 sentences

Each citing sentence is taken from the citing paper's LaTeX source and typed by Pith's classifier. A label appears at probability 0.8 or more (0.95 for support), a contest at 0.7 or more; the quoted words are the citing authors'. How each label was checked · JSON

Papers citing it · 16 sentences without a confident label

Uses its data or values 1 paper

For short GRBs, typically [ref] $E_iso ∼10^51$ erg, $M_ej ∼10^-5 M_⊙$, $θ_0 ∼10^∘$-$20^∘$.

Gamma-ray burst afterglow blast waves · Evolution of an expanding shell · 0.84

Compares with it 1 paper

The spatial profile of the deposition rate shows a quasi-universal power-law structure with a radial index of $-3$ to $-4$ within an opening angle of $30^∘$–$45^∘$, which is broadly consistent with the findings in the previous studies [ref] .

Neutrino pair annihilation driven jets from black-hole torus systems · Summary · 0.97

Cites it as background 4 papers

Details about how the black hole or disk drives the radiation, such as via electromagnetic Poynting flux [ref] or thermal energy deposition originated by neutrino-antineutrino annihilation [ref] , remain uncertain.

Gravitational and electromagnetic outputs from binary neutron star mergers · Introduction · 0.85
BNS and NSBH mergers could produce black holes (BHs) or neutron stars (NSs, in the case of BNSs) as the central engines that power GRBs [ref] .

Inferring Neutron Star Nuclear Properties from Gravitational-Wave and Gamma-Ray Burst Observations · Introduction · 0.88
Neutrino emission is important in mergers involving neutron star [ref] , the dense accretion disks of Gamma Ray Bursts (GRB) models [ref] , type Ia supernovae [ref] and X-ray flashes [ref] .

Nuclear Statistical Equilibrium neutrino spectrum · Introduction · 0.84

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