Vibes is a new algorithm that extracts physically motivated core structures from numerical star formation simulations by applying the virial theorem iteratively around density peaks to determine boundaries from energy balance rather than user-set density thresholds.
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11 Pith papers cite this work, alongside 1,507 external citations. Polarity classification is still indexing.
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representative citing papers
Self-regulating AGN jets in MHD simulations of cool-core clusters yield realistic FRI radio morphologies viewed along the jet axis and account for frequency-independent lobe extents via 1-50 μG fields allowing both young and old electrons to radiate.
Cellular Sheaf Neural Operators use cell complexes, learned restriction maps, and structure-aware message passing to create discretization-aware neural surrogates that preserve constraints in multiphysics PDEs such as MHD.
Advection-only galactic wind models fail to reproduce observed vertical radio profiles without unrealistic velocities, synchrotron spectra are biased toward young electrons in dense regions, and bremsstrahlung/Coulomb losses cannot be neglected even when subdominant.
In idealised driven subsonic MHD boxes, Arepo, Athena and Ramses all show dynamo amplification whose residual differences are explained by numerical diffusion, with no systematic advantage of constrained transport.
In AWSoM, switching from a non-conservative to a conservative energy equation raises CME kinetic energy by 232%, with hotter current-sheet pressure prolonging reconnection.
Dedner's mixed divergence cleaning produces substantial artifacts for strongly localized magnetic fields or sudden timestep changes; constrained transport is more accurate, and some prior early-Universe amplification claims may be affected.
Electron cooling exobase position organizes Rosetta ion-density regimes at 67P and requires inclusion in near-nucleus models to avoid underestimating densities.
Presents 24 AREPO+IllustrisTNG zoom-in simulations of clusters above 10^15 solar masses showing converged magnetic fields with volume-averaged plasma beta approximately 100 inside R200 after z~1.2, declining Faraday rotation profiles, and intermittent Braginskii heating approaching cooling rates in
Simulations of collapsing cores find that ε_ff varies with core definition via density threshold, open vs closed boundaries, and initial density, with higher values in low-mass cores due to lower infall rates.
Adapts FLASH code for MHD rigid body simulations to model non-magnetized planet-stellar wind interactions and examine viscosity influence on flow patterns.
citing papers explorer
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Virial-based extraction of structures in numerical simulations: The vibes tool
Vibes is a new algorithm that extracts physically motivated core structures from numerical star formation simulations by applying the virial theorem iteratively around density peaks to determine boundaries from energy balance rather than user-set density thresholds.
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Simulating realistic radio morphologies of Fanaroff-Riley I jets in a self-regulating cool-core cluster
Self-regulating AGN jets in MHD simulations of cool-core clusters yield realistic FRI radio morphologies viewed along the jet axis and account for frequency-independent lobe extents via 1-50 μG fields allowing both young and old electrons to radiate.
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Cellular Sheaf Neural Operators for Structure-Preserving Surrogate Modeling of Constrained PDEs
Cellular Sheaf Neural Operators use cell complexes, learned restriction maps, and structure-aware message passing to create discretization-aware neural surrogates that preserve constraints in multiphysics PDEs such as MHD.
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Revisiting radio synchrotron diagnostics in star-forming galaxies
Advection-only galactic wind models fail to reproduce observed vertical radio profiles without unrealistic velocities, synchrotron spectra are biased toward young electrons in dense regions, and bremsstrahlung/Coulomb losses cannot be neglected even when subdominant.
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A comparison of numerical schemes for driven subsonic MHD turbulence
In idealised driven subsonic MHD boxes, Arepo, Athena and Ramses all show dynamo amplification whose residual differences are explained by numerical diffusion, with no systematic advantage of constrained transport.
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The Effects of Energy Conservation in Simulating Solar Eruptions
In AWSoM, switching from a non-conservative to a conservative energy equation raises CME kinetic energy by 232%, with hotter current-sheet pressure prolonging reconnection.
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Systematic Comparison between Constrained Transport and Mixed Divergence Cleaning Methods for Astrophysical Magnetohydrodynamic Simulations
Dedner's mixed divergence cleaning produces substantial artifacts for strongly localized magnetic fields or sudden timestep changes; constrained transport is more accurate, and some prior early-Universe amplification claims may be affected.
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Cometary ion dynamics at a weakly outgassing comet
Electron cooling exobase position organizes Rosetta ion-density regimes at 67P and requires inclusion in near-nucleus models to avoid underestimating densities.
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The PICO-Cluster Project: presenting the galaxy cluster sample and studying magnetic field growth, Faraday rotation and Braginskii heating
Presents 24 AREPO+IllustrisTNG zoom-in simulations of clusters above 10^15 solar masses showing converged magnetic fields with volume-averaged plasma beta approximately 100 inside R200 after z~1.2, declining Faraday rotation profiles, and intermittent Braginskii heating approaching cooling rates in
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The efficiency per free-fall time as a ratio of the Star Formation Rate to the gas-infall rate in collapsing cores: dependence on the core definition, accretion, and radial structure
Simulations of collapsing cores find that ε_ff varies with core definition via density threshold, open vs closed boundaries, and initial density, with higher values in low-mass cores due to lower infall rates.
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Simulating the interaction of a non-magnetized planet with the stellar wind produced by a sun-like star using the FLASH Code
Adapts FLASH code for MHD rigid body simulations to model non-magnetized planet-stellar wind interactions and examine viscosity influence on flow patterns.