Turbulent magnetic field amplification in binary neutron star mergers

Palenzuela, C.; Aguilera-Miret, R.; Carrasco, F.; Ciolfi, R.; Kalinani, J. V.; Kastaun, W.; Miñano, B.; Viganò, D.

doi:10.48550/arxiv.2112.08413

Cited by 7 publications

(24 citation statements)

References 70 publications

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“…There have been a series of systematic numerical studies of the effect of magnetic fields on NSNS mergers (see e.g. [15,[18][19][20][21][22][23][24][25][26][27][28][29][30] and references therein). In particular, we have shown that NSNS remnants consisting of a BH + disk can launch a collimated, mildly relativistic outflow-an incipient jet-with duration and luminosity consistent with typical sGRB central engine lifetimes and magnitudes, as well as with the Blandford-Znajek mechanism [31] (hereafter BZ) for launching jets and their associated Poynting luminosities [26,32].…”

Section: Introductionmentioning

confidence: 99%

Jet Launching from Binary Neutron Star Mergers: Incorporating Neutrino Transport and Magnetic Fields

Sun,

Ruiz,

Shapiro

et al. 2022

Preprint

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We perform general relativistic, magnetohydrodynamic (GRMHD) simulations of merging binary neutron stars incorporating neutrino transport and magnetic fields. Our new radiative transport module for neutrinos adopts a general relativistic, truncated-moment (M1) formalism. The binaries consist of two identical, irrotational stars modeled by the SLy nuclear equation of state (EOS). They are initially in quasicircular orbit and threaded with a poloidal magnetic field that extends from the stellar interior into the exterior, as in typical pulsars. We insert neutrino processes shortly after the merger and focus on the role of neutrinos in launching a jet following the collapse of the hypermassive neutron star (HMNS) remnant to a spinning black hole (BH). We treat two microphysical versions: one (a "warm-up") evolving a single neutrino species and considering only charged-current processes, and the other evolving three species (νe, νe, νx) and related processes. We trace the evolution until the system reaches a quasiequilibrium state after BH formation. We find that the BH + disk remnant eventually launches an incipient jet. The electromagnetic Poynting luminosity is ∼ 10 53 erg s −1 , consistent with that of typical short gamma-ray bursts (sGRBs). The effect of neutrino cooling shortens the lifetime of the HMNS, and lowers the amplitude of the major peak of the gravitational wave (GW) power spectrum somewhat. After BH formation, neutrinos help clear out the matter near the BH poles, resulting in lower baryon-loaded surrounding debris. The neutrino luminosity resides in the range ∼ 10 52−53 erg s −1 once quasiequilibrium is achieved. Comparing with the neutrino-free models, we observe that the inclusion of neutrinos yields similar ejecta masses and is inefficient in carrying off additional angular momentum.

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Section: Introductionmentioning

confidence: 99%

Jet Launching from Binary Neutron Star Mergers: Incorporating Neutrino Transport and Magnetic Fields

Sun,

Ruiz,

Shapiro

et al. 2022

Preprint

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“…We present details of the latest version of the publicly available Mhduet code, which has previously been used to study phase transitions occurring in merging binaries [27] and, separately, magnetized mergers using the LES techniques [22][23][24][25][26]. Here we merge these efforts and extend the code to adopt realistic, finite temperature, tabulated equations of state along with neutrino cooling via the leakage scheme previously implemented in our other code, HAD [16,17,28].…”

Section: Evolution Systemmentioning

confidence: 99%

“…Beginning with the equations of motion for the MHD quantities expressed in Eqs. (25)(26)(27)(28), one would normally adopt a new notion for the corresponding filtered values of these conserved values. However, here we retain the same letters for each quantity where each implicitly represents the corresponding filtered value (i.e., simply resolved by the discretized equations, as in any simulation) within the LES approach.…”

Section: Large Eddy Simulationmentioning

confidence: 99%

“…where the fluxes and sources can be read easily from the standard GRMHD equations Eqs. (25)(26)(27)(28). The filtering procedure introduces additional (sub-filtered-scale) flux terms, which can be computed using the gradient SGS model, namely…”

Section: Large Eddy Simulationmentioning

confidence: 99%

“…To this end, we report on simulations and tests of Mhduet , which can now evolve the merger of magnetized neutron stars along with neutrino cooling using realistic, temperature-dependent, tabulated equations of state. To be more specific, this code leverages the recently developed large eddy simulation (LES) techniques [22][23][24][25][26] to study the growth of the magnetic field during and after the neutron star merger. A new method of computing the optical depth, extending the method first introduced in Ref.…”

Section: Introductionmentioning

confidence: 99%

See 2 more Smart Citations

Large Eddy Simulations of Magnetized Mergers of Neutron Stars with Neutrinos

Palenzuela,

Liebling,

Miñano

2022

Preprint

Self Cite

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Neutron star mergers are very violent events involving extreme physical processes: dynamic, strong-field gravity, large magnetic field, very hot, dense matter, and the copious production of neutrinos. Accurate modeling of such a system and its associated multi-messenger signals, such as gravitational waves, short gamma ray burst, and kilonova, requires the inclusion of all these processes, and is increasingly important in light of advancements in multi-messenger astronomy generally, and in gravitational wave astronomy in particular (such as the development of thirdgeneration detectors). Several general relativistic codes have been incorporating some of these elements with different levels of realism. Here, we extend our code Mhduet , which can perform large eddy simulations of magnetohydrodynamics to help capture the magnetic field amplification during the merger, and to allow for realistic equations of state and neutrino cooling via a leakage scheme. We perform several tests involving isolated and binary neutron stars demonstrating the accuracy of the code.

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The non-trivial magnetic configuration in neutron stars

Viganò

2020

Proc. IAU

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While predominantly dipolar, large-scale magnetic fields are usually assumed in most studies involving neutron stars, there are multiple observational, theoretical hints and numerical simulations highlightening the importance of non-dipolar components. I review here the most important observational facts and numerical studies pointing towards the existence of magnetospheric currents and internal small-scale structures, arising from multipoles of poloidal and toroidal fields. This holds for all neutron star stages: at birth, during their lifetime and after a merger.

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Turbulent magnetic field amplification in binary neutron star mergers

Cited by 7 publications

References 70 publications

Jet Launching from Binary Neutron Star Mergers: Incorporating Neutrino Transport and Magnetic Fields

Jet Launching from Binary Neutron Star Mergers: Incorporating Neutrino Transport and Magnetic Fields

Large Eddy Simulations of Magnetized Mergers of Neutron Stars with Neutrinos

The non-trivial magnetic configuration in neutron stars

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