Shock detection in meshless finite mass hydrodynamic schemes
Abstract
Shocks are prevalent in a multitude of astrophysical plasmas. They are essential in the dissipation of gravitational potential energy during structure formation, where they channel it into heat, turbulence, magnetic fields, and particle acceleration. Accurately capturing shocks in simulations of cosmological structure formation is a considerable challenge, due to the complexity of overlapping and colliding shocks, embedded in a medium experiencing complex shear flows. Fully Lagrangian hydrodynamical methods have historically been inferior in this regard compared to Eulerian or pseudo-Lagrangian methods. This work aims to remedy this discrepancy. We present the first efforts to implement a shockfinder algorithm with shock surface reconstruction for meshless finite mass (MFM) hydrodynamic schemes. We show its accuracy compared to analytic predictions and a legacy smoothed particle hydrodynamics (SPH)- based shock-finding method. We apply this new shock-finding method to simulations of cosmic structure formation to obtain improved predictions for shock energy dissipation and cosmic ray (CR) acceleration.
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BibTeX
@misc{boss2026shock,
title = {{Shock detection in meshless finite mass hydrodynamic schemes}},
author = {Ludwig M. Böss and Frederik Groth and Klaus Dolag and Damiano Caprioli},
howpublished = {arXiv},
year = {2026},
month = oct,
doi = {10.48550/arxiv.2610.38700},
eprint = {2610.38700},
archivePrefix = {arXiv},
url = {https://arxiv.org/abs/2610.38700},
note = {CC0},
}
RIS
TY - UNPB
TI - Shock detection in meshless finite mass hydrodynamic schemes
AU - Ludwig M. Böss
AU - Frederik Groth
AU - Klaus Dolag
AU - Damiano Caprioli
PY - 2026
DA - 2026/10/28
PB - arXiv
DO - 10.48550/arxiv.2610.38700
UR - https://arxiv.org/abs/2610.38700
AB - Shocks are prevalent in a multitude of astrophysical plasmas. They are essential in the dissipation of gravitational potential energy during structure formation, where they channel it into heat, turbulence, magnetic fields, and particle acceleration. Accurately capturing shocks in simulations of cosmological structure formation is a considerable challenge, due to the complexity of overlapping and colliding shocks, embedded in a medium experiencing complex shear flows. Fully Lagrangian hydrodynamical methods have historically been inferior in this regard compared to Eulerian or pseudo-Lagrangian methods. This work aims to remedy this discrepancy. We present the first efforts to implement a shockfinder algorithm with shock surface reconstruction for meshless finite mass (MFM) hydrodynamic schemes. We show its accuracy compared to analytic predictions and a legacy smoothed particle hydrodynamics (SPH)- based shock-finding method. We apply this new shock-finding method to simulations of cosmic structure formation to obtain improved predictions for shock energy dissipation and cosmic ray (CR) acceleration.
ER -