Mingxuan Liu 刘明轩
PhD Candidate · Department of Astronomy · University of Michigan
I am a third-year PhD candidate in the Department of Astronomy at the University of Michigan, working with Mateusz Ruszkowski. I work on plasma astrophysics: how turbulence, magnetic fields and cosmic rays move energy around in galaxies and galaxy clusters, and what that does to the gas.
Almost all of it is simulation. One strand is particle acceleration in turbulence driven by sheared flow, published in ApJ in 2026. In a newly completed manuscript on multiphase turbulence, we show how Ohmic and viscous dissipation concentrate heat in cold filaments, helping sustain gas near 104 K in cluster cores. The third is cosmic-ray transport, which I am starting now: measuring the scattering rate that sets how strongly cosmic rays couple to gas, rather than assuming it the way feedback models currently have to.
Before Michigan I was an undergraduate at Emory University, working with Elizabeth P. Hicks on Rayleigh–Taylor unstable flames. As a first-year there I also translated Janna Levin’s Black Hole Survival Guide into Chinese; it was published in 2022 and is rated 8.6 on Douban. I teach introductory astronomy at Michigan, and I have a husky named Vanilla.
Plasma astrophysics, magnetohydrodynamics, cosmic-ray acceleration and transport, turbulence, multiphase gas, hydrodynamic instabilities, numerical methods, HPC and physics-informed neural networks.
News
What I work on
These all come back to the same thing: how ordered flow in a fluid or plasma breaks down, and where the energy ends up.
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Cosmic-ray transport and feedback
Measuring the scattering rate that sets how far cosmic rays travel and how hard they push on gas, instead of putting it in by hand.
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Heating filaments in multiphase turbulence
How Ohmic and viscous dissipation concentrate turbulent energy in cold Hα filaments. New manuscript, an evolution movie and an interactive simulation viewer.
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Particle acceleration in shear-driven turbulence
MHD particle-in-cell simulations of a Kelvin–Helmholtz layer, following the particles the turbulence energizes. Published in ApJ 1009, 247 (2026).
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Rayleigh–Taylor unstable flames
Two perturbation modes on a model flame front. Which of five growth behaviors you get depends on GCD(k1, k2). Undergraduate work.