Introduces an adjoint projection method using volume-weighted metric to control numerical ∇·B errors in SPMHD, achieving roundoff-level accuracy with 1-10% overhead and consistent physical structures versus divergence cleaning.
Journal of Computational Physics , year = 2002, month = jan, volume =
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A Runge-Kutta-Gegenbauer super-time-stepping method for stable, efficient handling of anisotropic non-ideal MHD diffusion.
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.
Special relativistic simulations predict detectable radio emission from nightside magnetic structures around planets in pulsar winds, including for the known planet PSR J0636+5129 b.
3D MHD simulations show high-thrust, magnetically stabilized jets reach 5 Mpc in 15 Myr while weaker jets disrupt at ~3 Mpc over 35 Myr.
3D RMHD simulations with hybrid particle tracking reproduce the weak radio and strong X-ray redshift evolution in AGN jets via IC/CMB, including the (1+z)^4 X-ray scaling and the alpha-z relation.
Lagrangian tracers show mixing with low-entropy seeds drives most condensation in cluster cores; magnetic fields cause earlier divergence, higher vorticity, lower Mach numbers, and slower cold-cloud motion via tension.
Non-force-free initial magnetic fields in solar flare simulations release about twice the magnetic energy and yield EUV emission closer to observations than conventional NLFF extrapolations.
Stereoscopic HXR and EOVSA microwave data constrain source heights in a data-driven MHD simulation of the 2024 Oct 1 X7.1 flare, confirming consistency and associating a secondary source with southward reconnection in a current sheet that exhibits a higher electron low-energy cutoff.
Constrained transport outperforms Dedner's divergence cleaning in MHD simulations by avoiding spurious artifacts when magnetic fields are localized or timesteps vary suddenly.
Numerical MHD and test-particle simulations indicate that unsteady loop-top dynamics enhance electron acceleration efficiency compared to quasi-steady cases by mitigating betatron cooling at compressed field edges.
Relativistic MHD simulations of jet-driven shocks in post-merger ejecta show the GW-EM delay depends weakly on viewing angle and opacity, with a choked-jet model best matching GRB 170817A luminosity, delay, and duration.
Observational data-driven MHD simulations reproduced an X1.6 flare's onset and showed that photospheric velocity input extends prediction lead time beyond one hour.
3D MHD simulations of young massive star clusters find proton acceleration to hundreds of TeV near O-star termination shocks, with even faster acceleration to over 100 TeV in under 100 years when a supernova remnant expands inside the core.
GPU port of entropy-stable DG Euler solver with non-conservative buoyancy terms reaches nearly 70% of 64-bit peak on A100 volume kernels, delivers 10x speedup and 13x better energy efficiency versus CPU, and preserves symmetry-based flux savings.
Implements advanced GRMHD numerical techniques in Athena++ and demonstrates them via simulations of magnetically arrested disks around black holes.
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