Merging White Dwarf/Black Hole Binaries and Gamma‐Ray Bursts

Fryer, Chris L.; Woosley, S. E.; Herant, Marc; Davies, Melvyn B.

doi:10.1086/307467

Cited by 160 publications

(217 citation statements)

References 37 publications

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“…We start with a collapsing star, removing the assumption of "" stationarity ÏÏ (e.g., 1996), and follow the forJaroszynski mation of the accretion disk and itÏs subsequent evolution. While our paper will focus on the evolution of bare helium stars whose iron cores collapse to black holes, there are other ways of reaching similar initial conditions, especially the merger of a black hole with the helium core of red supergiant star following common-envelope evolution ; PWF) and white dwarfÈblack hole mergers (Fryer et al 1999b). Our model, though motivated by the desire to make a GRB, has the potential to create a strong supernova-like outburst or both.…”

Section: Introductionmentioning

confidence: 99%

Collapsars: Gamma‐Ray Bursts and Explosions in “Failed Supernovae”

MacFadyen

Woosley

1999

ApJ

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2,153

2,195

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Using a two-dimensional hydrodynamics code (PROMETHEUS), we explore the continued evolution of rotating helium stars, in which iron-core collapse does not produce a successful out-M a Z 10 M _ , going shock but instead forms a black hole of 2È3The model explored in greatest detail is the 14 M _ . helium core of a 35 main-sequence star. The outcome is sensitive to the angular momentum. M _ M _ For cm2 material falls into the black hole almost uninhibited. No outÑows are j 16 4 j/(1016 s~1) [ 3, expected. For the infalling matter is halted by centrifugal force outside 1000 km where neutrino j 16 Z 20, losses are negligible. The equatorial accretion rate is very low, and explosive oxygen burning may power a weak equatorial explosion. For however, a reasonable value for such stars, a compact 3 [ j 16 [ 20, disk forms at a radius at which the gravitational binding energy can be efficiently radiated as neutrinos or converted to beamed outÑow by magnetohydrodynamical (MHD) processes. These are the best candidates for producing gamma-ray bursts (GRBs). Here we study the formation of such a disk, the associated Ñow patterns, and the accretion rate for disk viscosity parameter a B 0.001 and 0.1. Infall along the rotational axis is initially uninhibited, and an evacuated channel opens during the Ðrst few seconds. Meanwhile the black hole is spun up by the accretion (to a B 0.9), and energy is dissipated in the disk by MHD processes and radiated by neutrinos. For the a \ 0.1 model, appreciable energetic outÑows develop between polar angles of 30¡ and 45¡. These outÑows, powered by viscous dissipation in the disk, have an energy of up to a few times 1051 ergs and a mass D1and are rich in 56Ni. They constitute M _ a supernova-like explosion by themselves. Meanwhile accretion through the disk is maintained for approximately 10È20 s but is time variable (^30%) because of hydrodynamical instabilities at the outer edge in a region where nuclei are experiencing photodisintegration. Because the efficiency of neutrino energy deposition is sensitive to the accretion rate, this instability leads to highly variable energy deposition in the polar regions. Some of this variability, which has signiÐcant power at 50 ms and overtones, may persist in the time structure of the burst. During the time followed, the average accretion rate for the standard a \ 0.1 and model is 0.07 s~1. The total energy deposited along the rotational j 16 \ 10 M _ axes by neutrino annihilation is (1È14) ] 1051 ergs, depending upon the evolution of the Kerr parameter and uncertain neutrino efficiencies. Simulated deposition of energy in the polar regions, at a constant rate of 5 ] 1050 ergs s~1 per pole, results in strong relativistic outÑow jets beamed to about 1% of the sky. These jets may be additionally modulated by instabilities in the sides of the "" nozzle ÏÏ through which they Ñow. The jets blow aside the accreting material, remain highly focused, and are capable of penetrating the star in D10 s. After the jet breaks through the surface of the sta...

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Section: Introductionmentioning

confidence: 99%

Collapsars: Gamma‐Ray Bursts and Explosions in “Failed Supernovae”

MacFadyen

Woosley

1999

ApJ

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2,153

2,195

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“…The early phases of a WD-NS merger have been previously studied as sources of gamma-ray bursts (Fryer et al 1999;King et al 2007;Paschalidis et al 2011) and SNlike optical transients (Metzger 2012;Fernández & Metzger 2013;MM16). The stages in the evolution of such systems are briefly summarized as follows (e.g.…”

Section: Introductionmentioning

confidence: 99%

“…If the ratio of the WD to the NS mass is sufficiently large (e.g., 0.2−0.5; Bobrick et al 2016), then mass transfer from the WD is unstable, and the ensuing phase of runaway accretion results in the WD being tidally disrupted (Verbunt & Rappaport 1988) into a thick and dense torus surrounding the NS (e.g. Fryer et al 1999). During the earliest stages of disk evolution (∼ minutes-hours), dynamically important nuclear burning occurs in the disk midplane (Metzger 2012).…”

Section: Introductionmentioning

confidence: 99%

Merger of a white dwarf–neutron star binary to 10²⁹carat diamonds: origin of the pulsar planets

Margalit

Metzger

2016

Mon. Not. R. Astron. Soc.

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We show that the merger and tidal disruption of a C/O white dwarf (WD) by a neutron star (NS) binary companion provides a natural formation scenario for the PSR B1257+12 planetary system. Starting with initial conditions for the debris disk produced of the disrupted WD, we model its long term viscous evolution, including for the first time the effects of mass and angular momentum loss during the early radiatively inefficient accretion flow (RIAF) phase and accounting for the unusual C/O composition on the disk opacity. For plausible values of the disk viscosity α ∼ 10 −3 − 10 −2 and the RIAF mass loss efficiency, we find that the disk mass remaining near the planet formation radius at the time of solid condensation is sufficient to explain the pulsar planets. Rapid rocky planet formation via gravitational instability of the solid carbon-dominated disk is facilitated by the suppression of vertical shear instabilities due to the high solid-to-gas ratio. Additional evidence supporting a WD-NS merger scenario includes (1) the low observed occurrence rate of pulsar planets ( 1% of NS birth), comparable to the expected WD-NS merger rate; (2) accretion by the NS during the RIAF phase is sufficient to spin PSR B1257+12 up to its observed 6 ms period; (3) similar models of 'low angular momentum' disks, such as those produced from supernova fallback, find insufficient mass reaching the planet formation radius. The unusually high space velocity of PSR B1257+12 of 326 km s −1 suggests a possible connection to the Calcium-rich transients, dim supernovae which occur in the outskirts of their host galaxies and were proposed to result from mergers of WD-NS binaries receiving SN kicks. The C/O disk composition implied by our model likely results in carbon-rich planets with diamond interiors.

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“…Several scenarios could lead to a black hole-massive accretion disk system. They include the merger of double-neutron star binaries (Eichler et al 1989;Ruffert et al 1997), neutron star-black hole binaries (Paczynski 1991;Janka et al 1999), black holewhite dwarf binaries (Fryer et al 1999b), and black holehelium star binaries (Fryer & Woosley 1998;Zhang & Fryer 2001).…”

Section: Introductionmentioning

confidence: 99%

“…On the other hand, those GRBs that have been unambiguously localized and identified (all of them long bursts with t e10 s) are likelier to be associated with massive stellar collapses (van Paradijs et al 2000). Numerical calculations of gravitational wave radiation from massive rotating stellar collapses have been done in the Newtonian approximation, for '' collapsar '' models of long GRBs in two dimensions (see, e.g., Fryer et al 1999b;McFadyen & Woosley 1999) and in three dimensions for general cases not intended as models for GRBs (Rampp, Muller, & Ruffert 1998). Recently, Dimmelmeier, Font, & Muller (2002) have performed relativistic simulations of rotational supernova core collapse in axisymmetry.…”

Section: Introductionmentioning

confidence: 99%

Gravitational Radiation from Gamma‐Ray Burst Progenitors

Kobayashi

Mészáros

2003

ApJ

126

164

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We study gravitational radiation from various proposed gamma-ray burst (GRB) progenitor models, in particular compact mergers and massive stellar collapses. These models have in common a high angular rotation rate, and the final stage involves a rotating black hole and accretion disk system. We consider the inspiral, merger, and ringing phases, and for massive collapses, we consider the possible effects of asymmetric collapse and break up, as well as bar-mode instabilities in the disks. We evaluate the orders of magnitude of the strain and frequency of the gravitational waves expected from various progenitors, at distances based on occurrence rate estimates. Based on simplifying assumptions, we give estimates of the probability of detection of gravitational waves by the advanced LIGO system from the different GRB scenarios.

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Merging White Dwarf/Black Hole Binaries and Gamma‐Ray Bursts

Cited by 160 publications

References 37 publications

Collapsars: Gamma‐Ray Bursts and Explosions in “Failed Supernovae”

Collapsars: Gamma‐Ray Bursts and Explosions in “Failed Supernovae”

Merger of a white dwarf–neutron star binary to 10²⁹carat diamonds: origin of the pulsar planets

Gravitational Radiation from Gamma‐Ray Burst Progenitors

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Merging White Dwarf/Black Hole Binaries and Gamma‐Ray Bursts

Cited by 160 publications

References 37 publications

Collapsars: Gamma‐Ray Bursts and Explosions in “Failed Supernovae”

Collapsars: Gamma‐Ray Bursts and Explosions in “Failed Supernovae”

Merger of a white dwarf–neutron star binary to 1029carat diamonds: origin of the pulsar planets

Gravitational Radiation from Gamma‐Ray Burst Progenitors

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Product

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Merger of a white dwarf–neutron star binary to 10²⁹carat diamonds: origin of the pulsar planets