Relativistic Jets in Collapsars

Zhang, Weiqun; Woosley, S. E.; MacFadyen, Andrew

doi:10.1086/367609

Cited by 453 publications

(519 citation statements)

References 40 publications

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“…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%

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

Aloy¹,

Janka²,

Müeller³

2005

A&A

254

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: 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

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“…LloydRonning et al (2004) showed that allowing the parameters of the jet profile to vary somewhat from burst to burst-the jet profile is now only quasi-universal-results both in variations in the value of E and deviations from a pure power law. While numerical modeling of hypernovae (Zhang et al 2003) shows that the surface energy density of the outflows should vary with off-axis angle, it does not predict the profile; thus, the profiles are fitted empirically to the data. Consequently, the observed E iso probability distribution is not a powerful discriminant between the two jet structure models.…”

Section: Introductionmentioning

confidence: 99%

Gamma‐Ray Burst Intensity Distributions

Band

Norris

Bonnell³

2004

ApJ

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We use the lag-luminosity relation to calculate self-consistently the redshifts, apparent peak bolometric luminosities L B , and isotropic energies E iso for a large sample of BATSE gamma-ray bursts. We consider two different forms of the lag-luminosity relation; for both forms the median redshift for our burst database is 1.6. We model the resulting E iso sample with power-law and Gaussian probability distributions without redshift evolution, both of which are reasonable models. The power-law model has an index of E ¼ 1:76 AE 0:05 (95% confidence), where p(E iso ) / E À E iso . The simple universal jet profile model suggested but did not require E ¼ 2, and subsequent physically reasonable refinements to this model permit greater diversity in E , as well as deviations from a power law; therefore, our observed E iso probability distribution does not disprove the universal jet model.

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“…A typical duration of a long GRB is a few tens of seconds, and in that time several solar masses are accreted by the black hole (Zhang et al 2003). Then, we adopṫ M = 0.1 M s −1 and q j = 0.02.…”

Section: Basic Modelmentioning

confidence: 91%

Neutrinos from collapsars

Vieyro

Romero

Peres

2013

A&A

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Context. Long gamma-ray bursts (GRBs) are associated with the gravitational collapse of very massive stars. The central engine of a GRB can collimate relativistic jets that propagate inside the stellar envelope. The shock waves produced when the jet disrupts the stellar surface are capable of accelerating particles up to very high energies. Aims. If the jet has hadronic content, neutrinos will be produced via charged pion decays. The main goal of this work is to estimate the neutrino emission produced in the region close to the surface of the star, taking pion and muon cooling into account, along with subtle effects arising from neutrino production in a highly magnetized medium. Methods. We estimate the maximum energies of the different kinds of particles and solve the coupled transport equations for each species. Once the particle distributions are known, we calculate the intensity of neutrinos. We study the different effects on the neutrinos that can change the relative weight of different flavors. In particular, we consider the effects of neutrino oscillations, and of neutrino spin precession caused by strong magnetic fields. Results. The expected neutrino signals from the shocks in the uncorking regions of Population III events is very weak, but the neutrino signal produced by Wolf-Rayet GRBs with z < 0.5 is not far from the level of the atmospheric background. Conclusions. The IceCube experiment does not have the sensitivity to detect neutrinos from the implosion of the earliest stars, but a number of high-energy neutrinos may be detected from nearby long GRBs. The cumulative signal should be detectable over several years (∼10 yr) of integration with the full 86-string configuration.

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Relativistic Jets in Collapsars

Cited by 453 publications

References 40 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

Gamma‐Ray Burst Intensity Distributions

Neutrinos from collapsars

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