GRChombo: An adaptable numerical relativity code for fundamental physics

Andrade, Tomás; Saló, Llibert Aresté; Aurrekoetxea, Josu C.; Bamber, Jamie; Clough, Katy; Croft, Robin; Eloy, de Jong,; Drew, Amelia; Durán, Alejandro; Ferreira, Pedro G.; Figueras, Pau; Finkel, Hal; Frana, Tiago; Ge, Bo-Xuan; Gu, Chenxia; Helfer, Thomas; Jäykkä, Juha; Joana, Cristian; Kunesch, Markus; Kornet, K.; Lim, Eugene A.; Muia, Francesco; Nazari, Zainab; Radia, Miren; Ripley, Justin L.; Shellard, P.; Sperhake, Ulrich; Traykova, Dina; Tunyasuvunakool, Saran; Wang, Zipeng; Widdicombe, James; Wong, Kaze W. K.

doi:10.21105/joss.03703

Cited by 67 publications

(36 citation statements)

References 68 publications

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“…We use an adapted version of the GRChombo numerical relativity framework [63][64][65] with the metric compo-nents and their derivatives calculated analytically at each point rather than stored on the grid. The evolution of the Proca field components follows the standard method of lines, with a fourth-order Runge-Kutta time integrator and fourth-order finite difference stencils.…”

Section: Numerical Details and Convergencementioning

confidence: 99%

The problem with Proca: ghost instabilities in self-interacting vector fields

Clough¹,

Helfer²,

Witek³

et al. 2022

Preprint

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Massive vector fields feature in several areas of particle physics, e.g., as carriers of weak interactions, dark matter candidates, or as an effective description of photons in a plasma. Here we investigate vector fields with self-interactions by replacing the mass term in the Proca equation with a general potential. We show that this seemingly benign modification inevitably introduces ghost instabilities of the same kind as those recently identified for vector-tensor theories of modified gravity (but in this simpler, minimally coupled theory). It has been suggested that nonperturbative dynamics may drive systems away from such instabilities. We demonstrate that this is not the case by evolving a self-interacting Proca field on a black hole background, where it grows due to the superradiant instability. The system initially evolves as in the massive case, but instabilities are triggered in a finite time once the self-interaction becomes significant. These instabilities have implications for the formation of condensates of massive, self-interacting vector bosons, the possibility of spin-one bosenovae, vector dark matter models, and effective models for interacting photons in a plasma.

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Section: Numerical Details and Convergencementioning

confidence: 99%

The problem with Proca: ghost instabilities in self-interacting vector fields

Clough¹,

Helfer²,

Witek³

et al. 2022

Preprint

Self Cite

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“…To numerically test the QFS system, given in Eq. ( 16), for angular momentum an example spacetime consisting of colliding boson stars is simulated in 3D using GRChombo [8,9]. GRChombo is a modern, open source, Numerical Relativity code with fully Adaptive Mesh Refinement (AMR) using the Berger-Rigoutsos blockstructured adaptive mesh algorithm [17].…”

Section: Numerical Applicationmentioning

confidence: 99%

“…Section IV is a standalone derivation of the well known Noether charge density from the QFS perspective and goes on to find the flux variable; results for complex scalar fields and complex Proca fields are given. The application of the QFS system to energy momentum currents, angular momentum and energy are given in section V. A fully non-linear test of the QFS system for angular momentum, using GRChombo [8,9] to perform Numerical Relativity simulations, is presented in section VI along with a convergence analysis.…”

Section: Introductionmentioning

confidence: 99%

Local Continuity of Angular Momentum and Noether Charge for Matter in General Relativity

Croft¹

2022

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“…A more detailed explanation of the structure and validation of code can be found in the appendix and in Ref. [67,72].…”

Section: A Computational Detailsmentioning

confidence: 99%

Gravitational dynamics in Higgs inflation: Preinflation and preheating with an auxiliary field

Joana

2022

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The dynamics of both the preinflationary and the preheating epochs for a model consisting of a Higgs inflaton plus an additional auxiliary field are studied in full General Relativity. The minimally coupled auxiliary field allows for parametric-type resonances that successfully transfer energy from the inflaton condensate to particle excitations in both fields. Depending on the interaction strengths of the fields, the broad resonance periods lead to structure formation consisting of large under/overdensities, and possibly the formation of compact objects. Moreover, when confronting the same model to multi-field inhomogeneous preinflation, the onset of inflation is shown to be a robust outcome. At relatively large Higgs values, the non-minimal coupling acts as a stabilizer, protecting the dynamics of the inflaton, and significantly reducing the impact of perturbations in other fields and matter sectors. These investigations further confirm the robustness of Higgs inflation to multifield inhomogeneous initial conditions, while putting in evidence the formation of complex structures during the reheating.

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GRChombo: An adaptable numerical relativity code for fundamental physics

Cited by 67 publications

References 68 publications

The problem with Proca: ghost instabilities in self-interacting vector fields

The problem with Proca: ghost instabilities in self-interacting vector fields

Local Continuity of Angular Momentum and Noether Charge for Matter in General Relativity

Gravitational dynamics in Higgs inflation: Preinflation and preheating with an auxiliary field

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