Neutrino Fast Flavor Conversions in Neutron-Star Postmerger Accretion Disks

Li, Xinyu; Siegel, Daniel M.

doi:10.1103/physrevlett.126.251101

Cited by 105 publications

(87 citation statements)

References 95 publications

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“…Monte-Carlo neutrino-radiation transport is also useful to incorporate pair annihilation (Foucart et al 2020). The other is the neutrino oscillation, which could modify nucleosynthetic yields for some part of the ejecta (Malkus et al 2012(Malkus et al , 2016Padilla-Gay et al 2021;Li and Siegel 2021). Its modeling will require us to address the challenging task of solving quantum kinetic equations in a dynamical spacetime (see, e.g., Richers et al 2019 for relevant work).…”

Section: Neutrino Emissionmentioning

confidence: 99%

Coalescence of black hole–neutron star binaries

2021

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We review the current status of general relativistic studies for coalescences of black hole–neutron star binaries. First, high-precision computations of black hole–neutron star binaries in quasiequilibrium circular orbits are summarized, focusing on the quasiequilibrium sequences and the mass-shedding limit. Next, the current status of numerical-relativity simulations for the merger of black hole–neutron star binaries is described. We summarize our understanding for the merger process, tidal disruption and its criterion, properties of the merger remnant and ejected material, gravitational waveforms, and gravitational-wave spectra. We also discuss expected electromagnetic counterparts to black hole–neutron star coalescences.

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Section: Neutrino Emissionmentioning

confidence: 99%

Coalescence of black hole–neutron star binaries

2021

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“…However, all these work have focused primarily on the inspiral to early merger stages, and hence, the long-term post-merger process has not been explored in these simulations. To compensate this drawback, many numerical simulations (viscous hydrodynamics or magnetohydrodynamics simulations) have been also performed for exploring long-term evolution of the accretion disks (or tori) around a black hole [51][52][53][54][55][56][57][58][59][60][61][62][63][64][65][66], and studied the post-merger mass ejection mechanisms and the properties of the post-merger ejecta.…”

Section: Introductionmentioning

confidence: 99%

General-relativistic neutrino-radiation magnetohydrodynamics simulation of black hole-neutron star mergers for seconds

Hayashi¹,

Fujibayashi²,

Kiuchi³

et al. 2021

Preprint

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Seconds-long numerical-relativity simulations for black hole-neutron star mergers are performed for the first time to obtain a self-consistent picture of the merger and post-merger evolution processes. To investigate the case that tidal disruption takes place, we choose the initial mass of the black hole to be 5.4M or 8.1M with the dimensionless spin of 0.75. The neutron-star mass is fixed to be 1.35M . We find that after the tidal disruption, dynamical mass ejection takes place spending 10 ms together with the formation of a massive accretion disk. Subsequently, the magnetic field in the disk is amplified by the magnetic winding and magnetorotational instability, establishing a turbulent state and inducing the angular momentum transport. The post-merger mass ejection by the magnetically-induced viscous effect sets in at ∼ 300-500 ms after the tidal disruption, at which the neutrino luminosity drops below ∼ 10 51.5 erg/s, and continues for several hundreds ms. A magnetosphere near the rotational axis of the black hole is developed after the matter and magnetic flux fall into the black hole from the accretion disk, and high-intensity Poynting flux generation sets in at a few hundreds ms after the tidal disruption. The intensity of the Poynting flux becomes low after the significant post-merger mass ejection, because the opening angle of the magnetosphere increases. The lifetime for the stage with the strong Poynting flux is 1-2 s, which agrees with the typical duration of short-hard gamma-ray bursts.

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“…The composition of the disk wind ejecta at a given time depends most sensitively on the instantaneous accretion rate (Siegel et al 2019). Following Siegel et al (2019), Miller et al (2020), and Li & Siegel (2021, we define the following accretion regimes:…”

Section: Collapsar Modelmentioning

confidence: 99%

“…As a result, the collapsar disk outflows, which feed on this neutronrich reservoir, can themselves possess a sufficiently high neutron concentration to enable an r-process, throughout much of the epoch over which the GRB jet is being powered. However, the details of the synthesized composition−particularly the partitioning between light and heavy r-process elements−are sensitive to the impact of neutrino absorption processes on the electron fraction of the outflowing material (Surman et al 2006;Miller et al 2020;Li & Siegel 2021).…”

Section: Introductionmentioning

confidence: 99%

"Super-Kilonovae" from Massive Collapsars as Signatures of Black-Hole Birth in the Pair-instability Mass Gap

Siegel¹,

Agarwal²,

Barnes³

et al. 2021

Preprint

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The core collapse of rapidly rotating massive ∼ 10M stars ("collapsars"), and resulting formation of hyper-accreting black holes, are a leading model for the central engines of long-duration gamma-ray bursts (GRB) and promising sources of r-process nucleosynthesis. Here, we explore the signatures of collapsars from progenitors with extremely massive helium cores 130M above the pair-instability mass gap. While rapid collapse to a black hole likely precludes a prompt explosion in these systems, we demonstrate that disk outflows can generate a large quantity (up to 50M ) of ejecta, comprised of 5 − 10M in r-process elements and ∼ 0.1 − 1M of 56 Ni, expanding at velocities ∼ 0.1 c. Radioactive heating of the disk-wind ejecta powers an optical/infrared transient, with a characteristic luminosity ∼ 10 42 erg s −1 and spectral peak in the near-infrared (due to the high optical/UV opacities of lanthanide elements) similar to kilonovae from neutron star mergers, but with longer durations 1 month. These "super-kilonovae" (superKNe) herald the birth of massive black holes 60M , whichas a result of disk wind mass-loss-can populate the pair-instability mass gap "from above" and could potentially create the binary components of GW190521. SuperKNe could be discovered via wide-field surveys such as those planned with the Roman Space Telescope or via late-time infrared follow-up observations of extremely energetic GRBs. Gravitational waves of frequency ∼ 0.1 − 50 Hz from non-axisymmetric instabilities in self-gravitating massive collapsar disks are potentially detectable by proposed third-generation intermediate and high-frequency observatories at distances up to hundreds of Mpc; in contrast to the "chirp" from binary mergers, the collapsar gravitational-wave signal decreases in frequency as the disk radius grows ("sad trombone").

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Neutrino Fast Flavor Conversions in Neutron-Star Postmerger Accretion Disks

Cited by 105 publications

References 95 publications

Coalescence of black hole–neutron star binaries

Coalescence of black hole–neutron star binaries

General-relativistic neutrino-radiation magnetohydrodynamics simulation of black hole-neutron star mergers for seconds

"Super-Kilonovae" from Massive Collapsars as Signatures of Black-Hole Birth in the Pair-instability Mass Gap

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