Addition of tabulated equation of state and neutrino leakage support to illinoisgrmhd

Werneck, Leonardo R.; Etienne, Z. B.; Murguia-Berthier, Ariadna; Haas, Roland; Cipolletta, Federico; Noble, Scott C.; Ennoggi, Lorenzo; Armengol, Federico G. Lopez; Giacomazzo, B.; Assumpção, Thiago; Faber, Joshua A.; Gupte, Tanmayee; Kelly, Bernard; Krolik, Julian H.

doi:10.1103/physrevd.107.044037

Cited by 11 publications

(8 citation statements)

References 143 publications

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“…While several numerical relativity simulations of magnetized binary neutron star mergers have been performed (e.g., Kiuchi et al 2014Kiuchi et al , 2022Dionysopoulou et al 2015;Palenzuela et al 2015Palenzuela et al , 2022Ciolfi et al 2017;Most et al 2019;Werneck et al 2023;Combi & Siegel 2023), turbulent magnetic field amplification during the collision (Price & Rosswog 2006;Kiuchi et al 2015;Aguilera-Miret et al 2020), which likely dominates the postmerger magnetic field geometry (Aguilera-Miret et al 2022), is not fully captured by current simulations (Kiuchi et al 2018). Although magnetic fields in the inspiral are not likely to strongly affect the orbital dynamics or gravitational-wave (GW) emission (Ioka & Taniguchi 2000;Zhu et al 2020), they could produce electromagnetic (EM) precursors prior to the merger (see, e.g., Hansen & Lyutikov 2001;Tsang et al 2012;Palenzuela et al 2013;Carrasco & Shibata 2020;Most & Philippov 2020, 2022aZhang 2020).…”

Section: Introductionmentioning

confidence: 99%

Flares, Jets, and Quasiperiodic Outbursts from Neutron Star Merger Remnants

Most¹,

Quataert²

2023

ApJL

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Using numerical relativity simulations with a subgrid dynamo prescription to generate strong initial magnetic fields, we investigate the possibility of launching a jet-like outflow from the hypermassive neutron star (HMNS) during the early stages of the merger, prior to the remnant’s collapse to a black hole. We demonstrate that buoyant instabilities in the strongly magnetized HMNS can lead to a periodic emission of powerful electromagnetic flares shortly after the merger. These are followed by a collimated mildly relativistic outflow. Both types of outflows feature quasiperiodic kilohertz substructure. These early-time outflows may power precursors to short-duration gamma-ray bursts (sGRBs) or in some cases the entire sGRB. While the overall temporal power spectrum we find broadly agrees with the one recently reported for quasiperiodic oscillations in the sGRB GRB910711, our simulations suggest that the periodic electromagnetic substructure is dominated by magnetohydrodynamic shearing processes rather than correlating with the corresponding postmerger gravitational-wave signal.

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Section: Introductionmentioning

confidence: 99%

Flares, Jets, and Quasiperiodic Outbursts from Neutron Star Merger Remnants

Most¹,

Quataert²

2023

ApJL

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“…For this reason, we divide our simulation of such events into two pieces. The first part is performed with the numerical relativity plus MHD code IllinoisGRMHD (Etienne et al 2015(Etienne et al , 2020Werneck et al 2023); the second part uses HARM3D+NUC (Murguia-Berthier et al 2021). A "hand-off" procedure assures consistency between the two in terms of the spacetime and the fluid properties (Lopez Armengol et al 2022).…”

Section: Overviewmentioning

confidence: 99%

“…The cooling rate  is the rate at which neutrinos (and antineutrinos) carry energy out of the gas. It is calculated from a local emission model and a leakage rate formalism (see Murguia-Berthier et al 2021;Werneck et al 2023, for details about the calculations of  and ).…”

Section: Physics Treated and Equations Solvedmentioning

confidence: 99%

“…The spacetime is evolved using Baikal (Haas et al 2022), while the MHD fields are evolved using a newly developed version of IllinoisGRMHD (Werneck et al 2023) that supports finite-temperature, microphysical EOSs, and neutrino physics via a leakage scheme. In addition to the MHD fields, we evolve the entropy by assuming that it is conserved (see, e.g., Noble et al 2009, for a similar strategy), an approximation that, while poor at shocks, allows us to use the entropy as a backup variable during primitive recovery (see Werneck et al 2023, for more details).…”

Section: Numerical Setupmentioning

confidence: 99%

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Bound Debris Expulsion from Neutron Star Merger Remnants

Zenati,

Krolik,

Werneck

et al. 2023

ApJ

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Many studies have found that neutron star mergers leave a fraction of the stars’ mass in bound orbits surrounding the resulting massive neutron star or black hole. This mass is a site of r-process nucleosynthesis and can generate a wind that contributes to a kilonova. However, comparatively little is known about the dynamics determining its mass or initial structure. Here we begin to investigate these questions, starting with the origin of the disk mass. Using tracer particle as well as discretized fluid data from numerical simulations, we identify where in the neutron stars the debris came from, the paths it takes in order to escape from the neutron stars’ interiors, and the times and locations at which its orbital properties diverge from those of neighboring fluid elements that end up remaining in the merged neutron star.

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“…The simplest and most inexpensive approach is the neutrino leakage scheme (see, e.g. Sekiguchi 2010, Deaton et al 2013, Palenzuela et al 2022a, Werneck et al 2023. This approximation seeks to account for changes in the electron fraction and in the energy losses due to the emission of neutrinos.…”

Section: Introductionmentioning

confidence: 99%

Global high-order numerical schemes for the time evolution of the general relativistic radiation magneto-hydrodynamics equations

Izquierdo

Pareschi

Miñano

et al. 2023

Class. Quantum Grav.

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Modeling correctly the transport of neutrinos is crucial in some astrophysical scenarios such as core-collapse supernovae and binary neutron star mergers. In this paper, we focus on the truncatedmoment formalism, considering only the ﬁrst two moments (M1 scheme) within the grey approximation, which reduces Boltzmann seven-dimensional equation to a system of 3+1 equations closely resembling the hydrodynamic ones. Solving the M1 scheme is still mathematically challenging, since it is necessary to model the radiation-matter interaction in regimes where the evolution equations become stiﬀ and behave as an advection-diﬀusion problem. Here, we present diﬀerent global, high-order time integration schemes based on Implicit-Explicit Runge-Kutta (IMEX) methods designed to overcome the time-step restriction caused by such behavior while allowing us to use the explicit RK commonly employed for the MHD and Einstein equations. Finally, we analyze their performance in several numerical tests.

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Addition of tabulated equation of state and neutrino leakage support to illinoisgrmhd

Cited by 11 publications

References 143 publications

Flares, Jets, and Quasiperiodic Outbursts from Neutron Star Merger Remnants

Flares, Jets, and Quasiperiodic Outbursts from Neutron Star Merger Remnants

Bound Debris Expulsion from Neutron Star Merger Remnants

Global high-order numerical schemes for the time evolution of the general relativistic radiation magneto-hydrodynamics equations

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