Production of<sup>56</sup>Ni in black hole-neutron star merger accretion disc outflows

Surman, Rebecca; Caballero, Oscar; McLaughlin, G. C.; Just, Oliver; Janka, Hans‐Thomas

doi:10.1088/0954-3899/41/4/044006

Cited by 23 publications

(30 citation statements)

References 36 publications

(62 reference statements)

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“…An important application of our results would in fact be to provide better initial conditions for long-term disk evolutions, or for nucleosynthesis studies requiring a detailed knowledge of the disk structure and composition (e.g. [83]). …”

Section: Discussionmentioning

confidence: 99%

Post-merger evolution of a neutron star-black hole binary with neutrino transport

et al. 2015

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We present a first simulation of the post-merger evolution of a black hole-neutron star binary in full general relativity using an energy-integrated general relativistic truncated moment formalism for neutrino transport. We describe our implementation of the moment formalism and important tests of our code, before studying the formation phase of an accretion disk after a black hole-neutron star merger. We use as initial data an existing general relativistic simulation of the merger of a neutron star of mass 1.4M with a black hole of mass 7M and dimensionless spin χBH = 0.8. Comparing with a simpler leakage scheme for the treatment of the neutrinos, we find noticeable differences in the neutron to proton ratio in and around the disk, and in the neutrino luminosity. We find that the electron neutrino luminosity is much lower in the transport simulations, and that both the disk and the disk outflows are less neutron-rich. The spatial distribution of the neutrinos is significantly affected by relativistic effects, due to large velocities and curvature in the regions of strongest emission. Over the short timescale evolved, we do not observe purely neutrino-driven outflows. However, a small amount of material (3 × 10 −4 M ) is ejected in the polar region during the circularization of the disk. Most of that material is ejected early in the formation of the disk, and is fairly neutron rich (electron fraction Ye ∼ 0.15 − 0.25). Through r-process nucleosynthesis, that material should produce high-opacity lanthanides in the polar region, and could thus affect the lightcurve of radioactively powered electromagnetic transients. We also show that by the end of the simulation, while the bulk of the disk remains neutron-rich (Ye ∼ 0.15 − 0.2 and decreasing), its outer layers have a higher electron fraction: 10% of the remaining mass has Ye > 0.3. As that material would be the first to be unbound by disk outflows on longer timescales, and as composition evolution is slower at later times, the changes in Ye experienced during the formation phase of the disk could have an impact on nucleosynthesis outputs from neutrino-driven and viscously-driven outflows. Finally, we find that the effective viscosity due to momentum transport by neutrinos is unlikely to have a strong effect on the growth of the magnetorotational instability in the post-merger accretion disk.

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Section: Discussionmentioning

confidence: 99%

Post-merger evolution of a neutron star-black hole binary with neutrino transport

et al. 2015

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“…For the role of weak interactions and resulting nucleosynthesis see e.g. [25,69,70]). The basic (consensus) picture is the following: explosion energies can be found up to 5 × 10 52 erg, 56 Ni ejecta up to 0.5 M ⊙ , and the ejecta are beamed with relativistic jets.…”

Section: Long Duration Gamma-ray Bursts and Hypernovaementioning

confidence: 99%

“…Optical and near-infrared observations of such an event, accompanying the short-duration GRB130603B have been reported [71] (see also [4]). After the first detailed nucleosynthesis predictions (following ideas of [33]) of such an event [13], many more and more sophisticated investigations have been undertaken, involving quite a number of authors [5,12,16,17,27,32,39,42,51,56,61,78] as well as the black hole accretion disk system after the formation of a central black hole [27,70,78,82].…”

Section: Neutron Star Mergersmentioning

confidence: 99%

Nucleosynthesis in Supernovae, Hypernovae/Gamma-ray Bursts and Compact Binary Mergers

Thielemann¹

2017

Proceedings of the 14th International Symposium on Nuclei in the Cosmos (NIC2016)

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We present the status and open problems of the astrophysical sites responsible for the nucleosynthesis of Fe-group and heavier elements (with the exception of the s-process). This involves type Ia supernovae with the requirement to have a low Y e -component (for the explanation of 55 Mn), the role of the core collapse supenova explosion mechanism in the composition of the Fe-group (and heavier?) ejecta, the transition between neutron star and black hole remnants as the result of the collapse of massive stars, and the relation of the latter with supernova and/or gamma-ray bursts / hypernovae. In addition, the role of compact binary mergers is discussed, especially with respect to forming the heaviest r-process elements in galactic eveolution.

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“…For the latter, the consideration of the 3D geometry of the source is of particular importance, as the relativistic effects (bending of neutrino trajectories and energy shifts) depend on the space-time curvature. In previous works [28,29], we have studied the influence of gravity on the emission of neutrinos and the production of heavy elements in outflows emerging from BH-AD via a post-processing of merger simulations and following neutrino trajectories in strong gravity.…”

Section: Introductionmentioning

confidence: 99%

Black hole spin influence on accretion disk neutrino detection

Caballero¹,

Zielinski²,

McLaughlin³

et al. 2016

Phys. Rev. D

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Neutrinos are copiously emitted from black hole accretion disks playing a fundamental role in their evolution, as well as in the production of gamma ray bursts and r-process nucleosynthesis. The black hole generates a strong gravitational field able to change the properties of the emerging neutrinos. We study the influence of the black hole spin on the structure of the neutrino surfaces, neutrino luminosities, average neutrino energies, and event counts at SuperK. We consider several disk models and provide estimates that cover different black hole efficiency scenarios. We discuss the influence of the detector's inclination with respect to the axis of the torus on neutrino properties. We find that tori around spinning black holes have larger luminosities, energies and rates compared to tori around static black holes, and that the inclination of the observer causes a reduction in the luminosities and detection rates but an increase in the average energies.PACS numbers: 26.50.+x, 26.30.Jk, 95.55Vj, 97.80.Gm, 97.10.Gz, 95.30.Sf

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Production of⁵⁶Ni in black hole-neutron star merger accretion disc outflows

Cited by 23 publications

References 36 publications

Post-merger evolution of a neutron star-black hole binary with neutrino transport

Post-merger evolution of a neutron star-black hole binary with neutrino transport

Nucleosynthesis in Supernovae, Hypernovae/Gamma-ray Bursts and Compact Binary Mergers

Black hole spin influence on accretion disk neutrino detection

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Production of56Ni in black hole-neutron star merger accretion disc outflows

Cited by 23 publications

References 36 publications

Post-merger evolution of a neutron star-black hole binary with neutrino transport

Post-merger evolution of a neutron star-black hole binary with neutrino transport

Nucleosynthesis in Supernovae, Hypernovae/Gamma-ray Bursts and Compact Binary Mergers

Black hole spin influence on accretion disk neutrino detection

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Production of⁵⁶Ni in black hole-neutron star merger accretion disc outflows