General relativistic hydrodynamics on a moving-mesh I: static space–times

Chang, Philip; Etienne, Z. B.

doi:10.1093/mnras/staa1532

Cited by 9 publications

(2 citation statements)

References 60 publications

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“…These elements make moving-mesh codes particularly interesting for simulating compact objects and in particular BNS systems. In recent years, some moving-mesh codes have been extended to include GRHD (Ryan & MacFadyen 2017;Chang & Etienne 2020). However, all these implementations currently employ a fixed spacetime, and to date no moving-mesh code evolves the spacetime dynamically, as it would for instance be required to simulate neutron star mergers.…”

Section: Introductionmentioning

confidence: 99%

General relativistic moving-mesh hydrodynamics simulations with AREPO and applications to neutron star mergers

Lioutas¹,

Bauswein²,

Soultanis³

et al. 2022

Preprint

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We implement general relativistic hydrodynamics in the moving-mesh code A . We also couple a solver for the Einstein field equations employing the conformal flatness approximation. The implementation is validated by evolving isolated static neutron stars using a fixed metric or a dynamical spacetime. In both tests the frequencies of the radial oscillation mode match those of independent calculations. We run the first moving-mesh simulation of a neutron star merger. The simulation includes a scheme to adaptively refine or derefine cells and thereby adjusting the local resolution dynamically. The general dynamics are in agreement with independent smoothed particle hydrodynamics and static-mesh simulations of neutron star mergers. Coarsely comparing, we find that dynamical features like the post-merger double-core structure or the quasi-radial oscillation mode persist on longer time scales, likely reflecting a lower numerical diffusivity of our method. Similarly, the post-merger gravitational wave emission shows the same features as observed in simulations with other codes. In particular, the main frequency of the post-merger phase is found to be in good agreement with independent results for the same binary system, while, in comparison, the amplitude of the post-merger gravitational wave signal falls off slower, i.e. the post-merger oscillations are less damped. The successful implementation of general relativistic hydrodynamics in the moving-mesh A code, including a dynamical spacetime evolution, provides a fundamentally new tool to simulate general relativistic problems in astrophysics.

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Section: Introductionmentioning

confidence: 99%

General relativistic moving-mesh hydrodynamics simulations with AREPO and applications to neutron star mergers

Lioutas¹,

Bauswein²,

Soultanis³

et al. 2022

Preprint

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show abstract

“…We use the moving-mesh hydrodynamic code, MANGA (Chang et al, 2017;Prust and Chang, 2019;Chang and Etienne, 2020), to simulate WDTDEs. MANGA solves the Euler equations with (self-)gravity, which written in conservative form are:…”

Section: Methodsmentioning

confidence: 99%

Numerical Simulations of White Dwarf Tidal Disruption Events

Humphrey

2023

Proc. Wisc. Space Conf.

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Numerical simulations of white dwarf tidal disruption events are performed using the 3-D moving-mesh hydrody- namic code, MANGA. In order to study the effect of nuclear burning on these events, we add a nuclear burning module to MANGA. Here, we present preliminary results from two simulations of white dwarf tidal disruption events with nuclear burning. We see no nuclear burning for shallow penetration (β = 2); however, we see significant nuclear burning for deep penetration (β = 5). Significant nuclear burning that produces radioactive elements will likely affect the light curve and observability of these events.

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The effect of impact parameter on tidal disruption events

Spaulding

Chang

2020

Monthly Notices of the Royal Astronomical Society

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Stars that pass too close to a supermassive black hole are disrupted by the black hole’s tidal gravity. Some debris is ejected while the remainder accretes into the black hole. To better study the physics of these debris, we use the moving mesh code MANGA to follow the evolution of the star from its initial encounter to its complete destruction. By varying the impact parameter (β) of the star, we study the energy distribution of the remaining material and the fallback rate of the material into the black hole as a function of time. We show that the spread of energy in the debris and peak luminosity time (tpeak) are both directly related to the impact parameter. In particular, we find a β1/2 scaling for the energy spread for β = 2 − 10 that levels off at β ≳ 10. We provide analytic arguments for the spread of energy, discuss implication of this scaling for the rise time of the light curve and broadness of the luminosity peak for these lower β’s. These relationships provide a possible means of inferring the impact parameters for observed TDEs.

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General relativistic hydrodynamics on a moving-mesh I: static space–times

Cited by 9 publications

References 60 publications

General relativistic moving-mesh hydrodynamics simulations with AREPO and applications to neutron star mergers

General relativistic moving-mesh hydrodynamics simulations with AREPO and applications to neutron star mergers

Numerical Simulations of White Dwarf Tidal Disruption Events

The effect of impact parameter on tidal disruption events

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