3D Relativistic Hydrodynamics

Aloy, M. A.; Martí, J.

doi:10.1007/3-540-46025-x_9

Cited by 3 publications

(3 citation statements)

References 144 publications

(174 reference statements)

Supporting

Mentioning

Contrasting

Order By: Relevance

“…12). Since they are radiation dominated the pressure variations effectively decouple from the density fluctuations (Aloy et al 2002). While the radiation pressure displays rather small variability across and along the fireball and falls almost monotonically about 15 orders of magnitude in the radial direction, the density variation in the same direction is more than 50 orders of magnitude and clearly non-monotonic (Fig.…”

Section: Dependence On the Half-opening Angle Of The Energy Depositiomentioning

confidence: 98%

“…The early phase of the propagation of jets in collapsars has been studied by nonrelativistic (MacFadyen & Woosley 1999;MacFadyen et al 2001) as well as special (Zhang & MacFadyen 2003) or general relativistic (Aloy et al 2000;Aloy & Martí 2002) hydrodynamic simulations in two dimensions (i.e., assuming axial symmetry). Also first axisymmetric magnetohydrodynamic simulations have been done for the formation of polar outflows from the central non-rotating BH in a collapsar in both Newtonian (Proga et al 2003; using a pseudoNewtonian potential, Pacyński & Wiita 1980) and general relativity (Mizuno et al 2004; assuming a fixed Schwarzshild metric).…”

Section: Introductionmentioning

confidence: 99%

See 1 more Smart Citation

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

Aloy¹,

Janka²,

Müeller³

2005

A&A

254

295

View full text Add to dashboard Cite

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).

show abstract

Section: Dependence On the Half-opening Angle Of The Energy Depositiomentioning

confidence: 98%

Section: Introductionmentioning

confidence: 99%

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

Aloy¹,

Janka²,

Müeller³

2005

A&A

254

295

View full text Add to dashboard Cite

show abstract

“…In such models the flow is kept hotter than in the present ones because of the occurrence of internal shocks already inside of the progenitor. However, since the outflow is optically thick, the thermal energy is not radiated away, but converted (later) into kinetic energy (Aloy et al 2000;Aloy& Martí 2002;Ghisellini et al 2007).…”

Section: Acceleration To High Lorentz Factormentioning

confidence: 99%

Angular Energy Distribution of Collapsar-Jets

Mizuta

Aloy

2009

ApJ

Self Cite

122

119

View full text Add to dashboard Cite

Collapsars are fast-spinning, massive stars, whose core collapse liberates an energy, that can be channeled in the form of ultrarelativistic jets. These jets transport the energy from the collapsed core to large distances, where it is dissipated in the form of long-duration gamma-ray bursts. In this paper we study the dynamics of ultrarelativistic jets produced in collapsars. Also we extrapolate our results to infer the angular energy distribution of the produced outflows in the afterglow phase. Our main focus is to look for global energetical properties which can be imprinted by the different structure of different progenitor stars. Thus, we employ a number of pre-supernova, stellar models (with distinct masses and metallicities), and inject in all of them jets with fixed initial conditions. We assume that at the injection nozzle, the jet is mildly relativistic (Lorentz factor ∼ 5), has a finite half-opening angle (5 • ), and carries a power of 10 51 erg s −1 . In all cases, well collimated jets propagate through the progenitor, blowing a high pressure and high temperature cocoon. These jets arrive intact to the stellar surface and break out of it. A large Lorentz factor region Γ > ∼ 100 develops well before the jet reaches the surface of the star, in the unshocked part of the beam, located between the injection nozzle and the first recollimation shock. These high values of Γ are possible because the finite opening angle of the jet allows for free expansion towards the radial direction. We find a strong correlation between the angular energy distribution of the jet, after its eruption from the progenitor surface, and the mass of the progenitors. The angular energy distribution of the jets from light progenitor models is steeper than that of the jets injected in more massive progenitor stars. This trend is also imprinted in the angular distribution of isotropic equivalent energy.

show abstract

Simulations of Jets from Active Galactic Nuclei and Gamma‐Ray Bursts

Aloy

Mimica

2012

Relativistic Jets From Active Galactic Nuclei

View full text Add to dashboard Cite

3D Relativistic Hydrodynamics

Cited by 3 publications

References 144 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

Angular Energy Distribution of Collapsar-Jets

Simulations of Jets from Active Galactic Nuclei and Gamma‐Ray Bursts

Contact Info

Product

Resources

About