Non-stationary hyperaccretion of stellar-mass black holes in three dimensions: torus evolution and neutrino emission

Setiawan, Sandi; Ruffert, M.; Janka, Hans‐Thomas

doi:10.1111/j.1365-2966.2004.07974.x

Cited by 89 publications

(135 citation statements)

References 24 publications

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“…This may lead to the acceleration of this matter to ultrarelativistic speeds, possibly accounting for a GRB with observed properties. If the duration of the event is related to the lifetime of the system (Sari & Piran 1997) this kind of events can only belong to the class of short GRBs because the expected timescale on which the black hole engulfs the disk is at most of a few hundred milliseconds Janka et al 1999;Lee & Ramirez-Ruiz 2002;Setiawan et al 2004).…”

Section: The Modelmentioning

confidence: 99%

“…We have further computed two models where the energy deposition rate was assumed to vary with time (models B07 and B08). These models were set up according to the following prescription for the energy deposition rate (guided by the results obtained by Setiawan et al 2004)…”

Section: The Case Of Low-density Halomentioning

confidence: 99%

“…In some of these models the energy deposition was taken constant up to 0.1 s and then switched off. In other models the energy deposition was modeled more "burst-like", reaching maximum values for a period of only 20 milliseconds and then decaying with time like a t −3/2 power law (cf., Setiawan et al 2004) or modulated during the whole evolution (including the decay phase) with a certain time variability of the energy released per unit of time. A summary of our main results and conclusions will follow in Sect.…”

Section: Introductionmentioning

confidence: 99%

“…These works have brought a theoretical understanding of the conditions that are present in the vicinity of the accreting BH and which determine the efficiency of energy loss by neutrino emission and the efficiency of energy conversion by neutrinoantineutrino annihilation. To this end, three-dimensional hydrodynamic simulations were performed by and more recently by Setiawan et al (2004) for the time-dependent accretion in BH-tori systems as the remnants of neutron star-neutron star (NS+NS) and NS+BH mergers. In this case the torus is not fed by an external mass reservoir as in case of a collapsar, and the timescale of BH accretion is determined by viscous transport in the torus, not by the collapse timescale of a massive star.…”

Section: Introductionmentioning

confidence: 99%

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

Aloy¹,

Janka²,

Müeller³

2005

A&A

253

295

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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 models of such mergers and future observations of short gamma-ray bursts by the SWIFT satellite. They show that ultrarelativistic outflow with maximum terminal Lorentz factors around 1000 develops for polar energy deposition rates above some 10 48 erg s −1 per steradian, provided the merger environment has a sufficiently low baryon density. By the interaction with the dense accretion torus the ultrarelativistic outflow with Lorentz factors Γ above 100 is collimated into a sharp-edged cone that is embedded laterally by a wind with steeply declining Lorentz factor. The typical semi-opening angles of the Γ > 100 cone are 5 • −10 • , corresponding to about 0.4−1.5% of the hemisphere and apparent isotropized energies (kinetic plus internal) up to ≈10 51 erg although at most 10−30% of the deposited energy is transferred to the outflow with Γ > 100. The viability of post-merger black hole-torus systems as engines of short, hard gamma-ray bursts is therefore confirmed. The annihilation of neutrino-antineutrino pairs radiated from the hot accretion torus appears as a suitable energy source for powerful axial outflow even if only ≈10 49 erg are deposited within a cone of 45 • half-opening angle around the system axis. Although the torus lifetimes are expected to be only between some 0.01 s and several 0.1 s, our models can explain the durations of all observed short gamma-ray bursts, because different propagation velocities of the front and rear ends will lead to a radial stretching of the ultrarelativistic fireball before transparency is reached. The ultrarelativistic flow reveals a highly non-uniform structure caused by the action of Kelvin-Helmholtz instabilities that originate at the fireball-torus interface. Large radial variations of the baryon density (up to several orders of magnitude) are uncorrelated with moderate variations of the Lorentz factor (factors of a few) and fluctuations of the gently declining radiation-dominated pressure. In the angular direction the Lorentz factor reveals a nearly flat plateau-like maximum with values of several hundreds, that can be located up to 7 • off the symmetry axis, and a steep decrease to less than 10 for polar angles larger than 15 • −20 • . Lateral expansion of the ultrarelativistic core of the flow is prevented by a subsonic velocity component of about 0.05c towards the symmetry axis, whereas the moderately relativistic wings show a subsonic sideways inflation with less than 0.07c (measured in the frame comoving with the radial flow).

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Section: The Modelmentioning

confidence: 99%

Section: The Case Of Low-density Halomentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

See 2 more Smart Citations

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

Aloy¹,

Janka²,

Müeller³

2005

A&A

253

295

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show abstract

“…Lee & Ramirez-Ruiz (2002) have analyzed the flow pattern within an accretion disk around a BH, and in recent papers (Lee et al 2004(Lee et al , 2005b) they included detailed microphysics in their simulations. Setiawan et al (2004) constructed disks around stellar mass black holes and followed their evolution, including explicit viscosity, while Rosswog et al (2004) investigated the dynamics of the accretion process.…”

Section: Introductionmentioning

confidence: 99%

Mergers of Neutron Star–Black Hole Binaries with Small Mass Ratios: Nucleosynthesis, Gamma‐Ray Bursts, and Electromagnetic Transients

Rosswog

2005

ApJ

301

325

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We discuss simulations of the coalescence of black hole-neutron star binary systems with black hole masses between 14 and 20 M . The calculations use a three-dimensional smoothed particle hydrodynamics code, a temperature-dependent, nuclear equation of state, and a multiflavor neutrino scheme. General relativistic effects are mimicked using the Paczyński-Wiita pseudo-potential and gravitational radiation reaction forces. Unlike previous, purely Newtonian calculations, in none of the explored cases does episodic mass transfer occur. The neutron star is always completely disrupted after most of its mass has been transferred directly into the hole. For black hole masses between 14 and 16 M an accretion disk forms; large parts of it, however, are inside the last stable orbit and therefore falling with large radial velocities into the hole. These disks are (opposite to the neutron star merger case) thin and-except for a spiral shock-essentially cold. For higher mass black holes (M BH ! 18 M ) almost the entire neutron star disappears in the hole without forming an accretion disk. In these cases the surviving material is spun up by tidal torques and ejected as a half-ring of neutron-rich matter. None of the investigated systems is a promising gamma-ray burst (GRB) central engine. We find between 0.01 and 0.2 M of the neutron star to be dynamically ejected. Like in a Type Ia supernova, the radioactive decay of this material powers a light curve with a peak luminosity of a few times 10 44 ergs s À1 . The maximum is reached about 3 days after the coalescence and is mainly visible in the optical/near-infrared band. The coalescence itself may produce a precursor pulse with a thermal spectrum of $10 ms duration.

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Three Little Pieces for Computer and Relativity

Rezzolla

2014

General Relativity, Cosmology and Astrophysics

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Abstract. Numerical relativity has made big strides over the last decade. A number of problems that have plagued the field for years have now been mostly solved. This progress has transformed numerical relativity into a powerful tool to explore fundamental problems in physics and astrophysics, and I present here three representative examples. These "three little pieces" reflect a personal choice and describe work that I am particularly familiar with. However, many more examples could be made.

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Non-stationary hyperaccretion of stellar-mass black holes in three dimensions: torus evolution and neutrino emission

Cited by 89 publications

References 24 publications

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

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

Mergers of Neutron Star–Black Hole Binaries with Small Mass Ratios: Nucleosynthesis, Gamma‐Ray Bursts, and Electromagnetic Transients

Three Little Pieces for Computer and Relativity

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