The Einstein Toolkit

Etienne, Z. B.; Brandt, Steven R.; Diener, Peter; Gabella, W.; Gracia-Linares, Miguel; Haas, Roland; Kedia, Atul; Alcubierre, Miguel; Alic, Daniela; Allen, Gabrielle; Ansorg, Marcus; Babiuc-Hamilton, Maria; Baiotti, Luca; Benger, Werner; Bentivegna, Eloisa; Bernuzzi, Sebastiano; Bode, Tanja; Bozzola, Gabriele; Brendal, Brockton; Bruegmann, Bernd; Campanelli, Manuela; Cipolletta, Federico; Corvino, Giovanni; Cupp, Samuel; Pietri, R. De; Dimmelmeier, Harry; Dooley, Rion; Dorband, Nils; Elley, Matthew; Khamra, Yaakoub El; Faber, Joshua A.; Font, Toni; Frieben, J.; Giacomazzo, B.; Goodale, Tom; Gundlach, Carsten; Hawke, Ian; Hawley, Scott H.; Hinder, Ian; Huerta, E. A.; Husa, S.; Iyer, Sai; Johnson, Daniel E.; Kellermann, Thorsten; Knapp, Andrew; Koppitz, Michael; Laguna, Pablo; Lanferman, Gerd; Löffler, Frank; Massó, Joan; Menger, Lars; Merzky, André; Miller, Jonah; Miller, Mark; Moesta, Philipp; Montero, Pedro J.; Mundim, Bruno C.; Nerozzi, Andrea; Noble, Scott C.; Ott, Christian D.; Paruchuri, Ravi; Pollney, Denis; Radice, David; Radke, Thomas; Reisswig, Christian; Rezzolla, Luciano; Rideout, David; Ripeanu, Matei; Sala, Lorenzo; Schewtschenko, J. A.; Schnetter, Erik; Schutz, Bernard F.; Seidel, E.; Seidel, Eric L.; Shalf, John; Sible, Ken; Sperhake, Ulrich; Stergioulas, Nikolaos; Suen, Wai-Mo; Szilágyi, Béla; Takahashi, Ryōji; Thomas, M.; Thornburg, Jonathan; Tobias, Malcolm; Tonita, Aaryn; Walker, Paul; Wan, Mew-Bing; Wardell, Barry; Werneck, Leonardo R.; Witek, Helvi; Zilhão, Miguel; Zink, Burkhard; Zlochower, Yosef

doi:10.5281/zenodo.3522086

Cited by 19 publications

(15 citation statements)

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“…Computational setup.-We simulate the long-term evolution of a typical post-merger accretion disk with the GRMHD code described in [34]. It represents an evolved version of GRHydro [35] and makes use of the Einstein Toolkit [36] [37][38][39][40][41]. We use the SFHo equation of state [42] as tabulated in Ref.…”

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confidence: 99%

Neutrino Fast Flavor Conversions in Neutron-Star Postmerger Accretion Disks

Siegel

2021

Phys. Rev. Lett.

105

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A compact accretion disk may be formed in the merger of two neutron stars or of a neutron star and a stellar-mass black hole. Outflows from such accretion disks have been identified as a major site of rapid neutron-capture (r-process) nucleosynthesis and as the source of 'red' kilonova emission following the first observed neutron-star merger GW170817. We present long-term generalrelativistic radiation magnetohydrodynamic simulations of a typical post-merger accretion disk at initial accretion rates of Ṁ ∼ 1 M s −1 over 400 ms post-merger. We include neutrino radiation transport that accounts for effects of neutrino fast flavor conversions dynamically. We find ubiquitous flavor oscillations that result in a significantly more neutron-rich outflow, providing lanthanide and 3rd-peak r-process abundances similar to solar abundances. This provides strong evidence that post-merger accretion disks are a major production site of heavy r-process elements. A similar flavor effect may allow for increased lanthanide production in collapsars. The formalism presented here may also be used in simulations of core-collapse supernovae to explore whether fast conversions strengthen or weaken the explosion.

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confidence: 99%

Neutrino Fast Flavor Conversions in Neutron-Star Postmerger Accretion Disks

Siegel

2021

Phys. Rev. Lett.

105

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“…The (1+log) and Gamma-driver gauge conditions are adopted for the evolution of lapse and shift (Alcubierre 2008;Baiotti & Rezzolla 2017). We use the M L code (Brown et al 2009) for evolution of spacetime variables which is a publicly available code in the E -T (Babiuc-Hamilton et al 2019;Goodale et al 2003;Schnetter et al 2006Schnetter et al , 2004…”

Section: Dynamical Evolutionmentioning

confidence: 99%

$f$-mode oscillations of compact stars in dynamical spacetimes: Equation of state dependencies and universal relations studies

Shashank,

Nouri,

Gupta

2021

Preprint

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In this article, we study the fundamental ( 𝑓 -)modes of non-rotating compact stars with realistic equations of state (EoS), extracted in the dynamical spacetime using numerical relativity simulations. We use a set of EoS with varying degree of stiffness and numerically evolve perturbed star models for several mass configurations (in the range of 1.2 − 2.0 𝑀 ) for each of these EoS. We find the 𝑓 -mode frequency being lower for the stiffer EoS. We also see the increase in the frequency for higher mass systems as compared to the smaller mass cases. While the increase is linear for 𝑀 ≤ 1.6𝑀 , it shows deviation from linearity with the sharper change and higher values of 𝑓 -modes for some of the EoS for more massive systems. We notice that the frequencies are distinguishable for soft, intermediate and stiffer EoS, thus it might be possible to constraint the EoS based on the detected signal frequency from the binary neutron star merger. More specifically for the softer EoSs, the 𝑓 -mode frequency is in the range of 1.8 − 2.2 kHz for the masses between 1.2 − 1.8𝑀 . On the other hand, in the case of stiffer EoS, such as 'BHB' and 'DD2' frequency is shifted to lower values 1.55 − 1.8 kHz for the same mass range.

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“…where N and β i are the lapse function and shift vector respectively. The resulting system is numerically evolved using the Einstein Toolkit infrastructure [30][31][32] with Carpet [33,34] for mesh-refinement capabilities and the multipatch infrastructure Llama [35]. The scalar field equations are evolved in time by adapting the ScalarEvolve code available in [36], which was first used and described in [37].…”

Section: A Numerical Implementationmentioning

confidence: 99%

Black hole binaries and light fields: Gravitational molecules

Ikeda,

Bernard,

Cardoso

et al. 2020

Preprint

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We show that light scalars can form quasi-bound states around binaries. In the non-relativistic regime, these states are formally described by the quantum-mechanical Schrödinger equation for a one-electron heteronuclear diatomic molecule. We performed extensive numerical simulations of scalar fields around black hole binaries showing that a scalar structure condensates around the binary -we dub these states "gravitational molecules". We further show that these are well-described by the perturbative, non-relativistic description.

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The Einstein Toolkit

Cited by 19 publications

References 0 publications

Neutrino Fast Flavor Conversions in Neutron-Star Postmerger Accretion Disks

Neutrino Fast Flavor Conversions in Neutron-Star Postmerger Accretion Disks

$f$-mode oscillations of compact stars in dynamical spacetimes: Equation of state dependencies and universal relations studies

Black hole binaries and light fields: Gravitational molecules

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