James R. Beattie

Numerical magnetohydrodynamics at the IAS

Mon, 01 Jan 0001 00:00:00 +0000

Bring a result, a paper, or a problem in magnetohydrodynamics. The emphasis is on discussion: working through the physics together, comparing approaches, and finding useful next steps.

Magnetogenesis

Mon, 01 Jan 0001 00:00:00 +0000

A meeting for questions about where magnetic fields come from and how they grow. Sessions can connect seed-field mechanisms, dynamo theory, numerical models, and observational constraints.

Example Talk

Sat, 01 Jun 2030 13:00:00 +0000

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Joining IAS as a NASA Hubble Fellow

Sat, 05 Sep 2026 00:00:00 +0000

This September, I’m joining the Institute for Advanced Study as a NASA Hubble Fellow and Member in the School of Natural Sciences.

My research explores how turbulence and magnetic fields evolve in astrophysical plasmas. At IAS, I will develop analytical and numerical models of how young supernova remnants drive and maintain turbulence in our Galaxy.

I look forward to new collaborations and conversations. Please get in touch if you would like to discuss turbulence, dynamos, or plasma astrophysics.

Residual energy in magnetized turbulence, published in A&A

Mon, 31 Aug 2026 00:00:00 +0000

Our paper, Residual energy in weakly compressible turbulence with a mean guide field, is published in Astronomy & Astrophysics, 713, A7. I worked with lead author Raphael Skalidis, Aris Tritsis, and Philip F. Hopkins.

Using simulations of weakly compressible turbulence with a strong mean magnetic field, we compare driving through velocity fluctuations with driving through magnetic fluctuations. The two methods produce different energy balances even at comparable sonic and Alfvénic Mach numbers.

Magnetic driving produces nearly equal kinetic and magnetic energies in the inertial range, while velocity driving leaves an excess of kinetic energy. Section 3 of the paper presents the numerical comparison, showing why the driving mechanism matters when interpreting magnetized turbulence.

Read the published paper or read the open preprint.

Fluid Theory, Turbulence, and Dynamos in Magnetized Plasmas

Wed, 05 Aug 2026 00:00:00 +0000

Contents

Fluid theory, waves, and instabilities.
Conservation laws for magnetized fluids.
Ideal-MHD waves and their restoring forces.
Rayleigh-Taylor instability.
Hydrodynamic turbulence.
Kolmogorov phenomenology, exact energy budgets, and intermittency.
Magnetohydrodynamic turbulence.
Elsasser variables, weak turbulence, critical balance, and dynamic alignment.
Fluid dynamos.
Kinematic and nonlinear small-scale dynamos.
Mean-field theory and large-scale dynamos.
Derivations and mathematical details.

SCEECS lecture notes are available

Wed, 05 Aug 2026 00:00:00 +0000

My notes from the 2026 SCEECS summer school, Fluid Theory, Turbulence, and Dynamos in Magnetized Plasmas, are now available on the website.

The notes cover fluid and magnetohydrodynamic theory, waves and instabilities, hydrodynamic and magnetized turbulence, and small- and large-scale dynamos, with derivations and mathematical details throughout.

Read the notes or download the PDF.

Visa Appointments

Thu, 02 Jul 2026 00:00:00 +0000

My single-author ApJL paper on supernova-driven turbulence

Wed, 03 Jun 2026 00:00:00 +0000

My single-author paper, Supernovae Drive Large-scale, Incompressible Turbulence through Small-scale Instabilities, is published in The Astrophysical Journal Letters, 1004, L9.

I study how individual supernova remnants generate incompressible turbulence. Instabilities wrinkle the interface between hot and warm gas, bringing pressure and density gradients out of alignment and generating vorticity. Vortex stretching then allows turbulent motions to escape the shell into the surrounding gas.

The result connects the structure of these thin interfaces to the wider galactic turbulence cascade: small-scale instabilities can supply turbulent motions that an inverse cascade carries to larger scales. Sections III and IV of the paper develop and test this mechanism.

Read the published paper, read the open preprint, or explore the science highlight.

Numerical simulations of shock-driven, supersonic turbulence in colliding three-temperature laboratory plasmas

Wed, 20 May 2026 00:00:00 +0000

What is the Strouhal number of turbulence driven by supernovae?

Tue, 05 May 2026 00:00:00 +0000

Compressible Navier--Stokes Flow in Schrödinger-Type Variables

Wed, 29 Apr 2026 00:00:00 +0000

Compressible Navier–Stokes flow in Schrödinger-type variables

Wed, 29 Apr 2026 00:00:00 +0000

Our paper, Compressible Navier–Stokes Flow in Schrödinger-Type Variables, is available on arXiv.

With Max Sokolova, Khush Negandhi, and Bart Ripperda, I derive an exact reformulation of isothermal compressible Navier–Stokes flow using Cole–Hopf-type transformations. The construction separates compressive, vortical, and density-carrying parts of the flow in two and three dimensions.

We test the transformed equations against a direct Kelvin–Helmholtz shear-layer simulation. The comparison is described in Section IV of the paper.

Update, September 2026: The paper is accepted in Physical Review Research, as noted in the current arXiv record.

Read the preprint, download the PDF, or view the science highlight.

Matt Sampson’s cosmic-ray study is published

Wed, 08 Apr 2026 00:00:00 +0000

Our study, Cosmic-Ray and Plasma Coupling for Isothermal Supersonic Turbulence in the Magnetized Interstellar Medium, led by Matt Sampson, is now published in The Astrophysical Journal, volume 1001, article 99 (April 2026).

The paper explores how cosmic rays and turbulent, magnetized plasma interact as the cosmic-ray diffusion and streaming properties vary. Congratulations, Matt, and thank you to all our collaborators!

Read the published paper or read the preprint.

Magnetic dynamos

Mon, 30 Mar 2026 00:00:00 +0000

Contents
Magnetic dynamos.
Goals for this lecture.
The induction equation.
Small-scale dynamo (kinematic only).
Magnetic energy spectrum evolution.
The Kazantsev (1968) k^(3/2) model.
Closure of the third-order correlators.
Diffusion-free regime.
Resistively truncated regime.
Comments.
Large-scale dynamo.
Mean-field induction equation and the EMF.
Exact fluctuation equation and the FOSA closure.
Scale expansion and isotropic reduction.
Derivation of alpha and beta under FOSA.
Why inhomogeneous mean flows are harder.
Inferring transport coefficients from data.
Some simple large-scale dynamos that may or may not exist.
The alpha^2 dynamo.
The alpha Omega dynamo.

A large-scale, vertical field driven dynamo from the Kelvin-Helmholtz instability: implications for merging compact objects and other thoughts

Thu, 05 Mar 2026 00:00:00 +0000

Supernova remnants as engines of non-Kolmogorov galactic turbulence (and why we need to throw away old ideas applied to ISM turbulence)

Thu, 05 Mar 2026 00:00:00 +0000

What do the world's largest simulations of cold phase interstellar medium turbulence tell us?

Thu, 05 Mar 2026 00:00:00 +0000

Can you create a large-scale vertical field from the KHI? Yup.

Wed, 25 Feb 2026 00:00:00 +0000

The PDF poster is available below.

Download full poster (PDF)

Supernova remnants as engines of non-Kolmogorov galactic turbulence

Wed, 18 Feb 2026 00:00:00 +0000

Kinetic to Viscous Fluid Model via First-Order Chapman-Enskog Expansion

Sun, 08 Feb 2026 00:00:00 +0000

Contents
Boltzmann equation and the BGK collision operator.
Zeroth-moment (mass conservation).
First-moment (momentum conservation).
Second-moment (energy conservation).
Chapman-Enskog expansion.
Zeroth-order: local equilibrium and Euler equations.
Isotropic pressure.
Vanishing heat flux.
First-order expression for f(1).
The zeroth-order material derivatives.
Partial Derivatives of the Maxwellian.
Moments of f(1): heat flux and pressure corrections.
Relevant first-order fluxes.
Decomposition of f(1) by tensorial parity.
First-order heat flux from odd terms of f(1) and Fourier’s law of heat conduction.
Pressure corrections and bulk viscosity from the isotropic, even terms of f(1).
Shear viscosity from the traceless, even terms of f(1).

Fluid moments and linear waves in ideal magnetohydrodynamics

Sat, 07 Feb 2026 00:00:00 +0000

Contents
Lecture goals.
Boltzmann equation for a monoatomic gas.
Zeroth-moment (mass conservation).
First-moment (momentum conservation).
Second-moment (energy conservation).
Isotropic pressure and moment closure.
Boltzmann equation for a non-relativistic, magnetized plasma.
From Boltzmann equation to an ideal MHD fluid.
Moments of the multi-species Boltzmann equation.
Ideal MHD equations.
The repercussions and assumptions of ideal MHD.
Linearization.
Small perturbations about a homogeneous equilibrium.
Linearization of the ideal MHD equations.
Linearized Continuity Equation.
Linearized Induction Equation.
Linearized Momentum Equation.
Plane-wave solutions.
Constructing the linear system.
Constructing the eigenvalue problem for u-hat.
Rearrange u-hat.
Rearrange rho-hat.
Rearrange B-hat.
Rebuilding u-hat in an appropriate form.
Ideal MHD Eigenmodes.
Alfven mode.
Fast and slow magnetosonic modes.
Limiting cases for propagation angle.
High- and low-beta limits.

Conservation of magnetic-helicity fluctuations due to spatial decorrelation of fluxes in decaying MHD turbulence

Sat, 01 Nov 2025 00:00:00 +0000

Why interstellar turbulence is non-Kolmogorov and how structures fit into turbulence phenomenology

Thu, 30 Oct 2025 00:00:00 +0000

So long Kolmogorov -- a supernovae-driven turbulence phenomenology

Wed, 01 Oct 2025 00:00:00 +0000

Fundamental Results from the World's Largest Simulation of Compressible MHD Turbulence

Sat, 20 Sep 2025 00:00:00 +0000

The growth of magnetic energy during the nonlinear phase of the subsonic and supersonic small-scale dynamo

Mon, 15 Sep 2025 00:00:00 +0000

Supernovae drive large-scale, incompressible turbulence through small-scale instabilities

Tue, 09 Sep 2025 00:00:00 +0000

Cascading from the winds to the disk: the universality of supernovae-driven turbulence in different galactic interstellar mediums

Mon, 01 Sep 2025 00:00:00 +0000

The chronology of high-k magnetic modes -- from dynamo to stationary turbulence

Mon, 01 Sep 2025 00:00:00 +0000

Live Publications

Sun, 27 Jul 2025 00:00:00 +0000

This page automatically displays my latest publications directly from the NASA Astrophysics Data System (ADS). The list updates automatically as new papers are added to ADS.

The widget below shows all publications where I am listed as an author, sorted by most recent first.

Magnetized supersonic turbulence with unprecedented dynamical range

Tue, 17 Jun 2025 00:00:00 +0000

Cosmic ray and plasma coupling for isothermal supersonic turbulence in the magnetized interstellar medium

Wed, 04 Jun 2025 00:00:00 +0000

Matt Sampson’s cosmic-ray and plasma-coupling study is on arXiv

Wed, 04 Jun 2025 00:00:00 +0000

Our study of cosmic-ray and plasma coupling, led by Matt Sampson, is available as a preprint on arXiv.

Update, April 2026: The paper is now published in The Astrophysical Journal.

Scale-dependent alignment in compressible magnetohydrodynamic turbulence

Thu, 22 May 2025 00:00:00 +0000

The spectrum of magnetized turbulence in the interstellar medium

Fri, 16 May 2025 00:00:00 +0000

🎉Published in Nature Astronomy🎉 -- The spectrum of magnetized turbulence in the interstellar medium!

Tue, 13 May 2025 00:00:00 +0000

🎉I've submitted our work on dynamical alignment to PRL!

Tue, 22 Apr 2025 00:00:00 +0000

No phenomenology is safe -- surprises from extreme Reynolds number MHD turbulence simulations

Mon, 14 Apr 2025 00:00:00 +0000

Comparison of magnetic diffusion and reconnection in ideal and resistive relativistic magnetohydrodynamics, ideal magnetodynamics and resistive force-free electrodynamics

Tue, 25 Mar 2025 00:00:00 +0000

Density Fluctuation–Mach Number Scaling in Compressible, High Plasma Beta Turbulence: In Situ Space Observations and High-Reynolds Number Simulations

Thu, 13 Mar 2025 00:00:00 +0000

The Three Phases of the KHI Dynamo

Sat, 01 Feb 2025 00:00:00 +0000

The PDF poster is available below.

Download full poster (PDF)

🎉Congrats Neco Kriel🎉 (ANU) -- student-led study published on the supersonic turbulent dynamo!

Fri, 31 Jan 2025 00:00:00 +0000

Fundamental MHD scales -- II: the kinematic phase of the supersonic small-scale dynamo

Fri, 31 Jan 2025 00:00:00 +0000

So long Kolmogorov: the forward and backward turbulence cascades in a supernovae-driven, multiphase interstellar medium

Mon, 20 Jan 2025 00:00:00 +0000

🎉My first SNe-driven turbulence paper is on the arXiv!

Thu, 16 Jan 2025 00:00:00 +0000

Magnetized supersonic turbulence sustained by a fluctuation dynamo

Wed, 09 Oct 2024 00:00:00 +0000

The interstellar cascade II - supernova driven turbulence

Wed, 25 Sep 2024 00:00:00 +0000

The interstellar cascade I - the world’s largest turbulent MHD box experiment

Mon, 23 Sep 2024 00:00:00 +0000

Off to Lyon and Chateau de Goutelas

Sat, 21 Sep 2024 00:00:00 +0000

🎉 I was a commentator in a CNN article on the Starry Night

Wed, 18 Sep 2024 00:00:00 +0000

🎉 ICM talk at Galaxy Clusters & Radio Relics II, Center for Astrophysics | Harvard & Smithsonian

Fri, 06 Sep 2024 00:00:00 +0000

From fast growth to saturation of the intracluster medium dynamo

Fri, 06 Sep 2024 00:00:00 +0000

Aspects of magnetic field growth and the turbulent dynamo

Mon, 19 Aug 2024 00:00:00 +0000

Characterising magnetic field structure across scales - X and O point detection in three dimensions

Mon, 19 Aug 2024 00:00:00 +0000

Reconnection and dynamo are fundamentally opposite plasma processes - reconnection describing the conversion of magnetic energy density into kinetic, and dynamo conversion of kinetic energy density into magnetic. Both processes however do share a similarity in that they change the underlying topology of the magnetic field. Utilising the structure of the magnetic field via the gradient tensor of the vector potential, magnetic field itself, or current density, one can identify and characterise objects like O and X points which can be used to directly probe the local properties of a reconnecting region in a turbulent plasma, or associate global properties, like integral magnetic energy growth, with specific local regions in the plasma. In this project, we will develop a method for characterising such topologies in 2D and 3D turbulent MHD plasma, relevant to the interstellar medium, and test fundamental questions about the nature of reconnection in such a regime. This will have significant implications for understanding the very nature of MHD turbulence in our Galaxy, and the role that reconnection may play.

Developing a turbulence-regulated star formation theory in a medium with non-lognormal gas density statistics.

Mon, 19 Aug 2024 00:00:00 +0000

Star formation happens within cold molecular clouds which are subject to supersonic turbulent motions and strong magnetic fields. The gas density PDF of such a medium has been previously used to predict the star formation rate potential that a cold gas cloud has, e.g., Krumholz & McKee (2005), Federrath & Klessen (2012) and Burkhart & Mocz (2018). Critical to these theories is the lognormal gas density probability density function, which connects the underlying statistics of the medium to the star formation rate in these models. However, foundational works from Hopkins (2013a), Mocz & Burkhart (2018) and Beattie et al (2022a) indicate that (global) lognormal models violate mass conservation, and are theoretically and empirically incorrect for the gas density probability density function of a supersonic medium. In this project, we aim to utilise computational and analytical techniques to modify the Federrath & Klessen (2012)-type turbulence-regulated star formation theories to include underlying Hopkins (2013a) gas density statistics, exploring how higher-order moments of the PDF influence the theoretical star formation rate. Furthermore, we will calibrate our theoretical models with star formation rates predicted by detailed numerical star-formation simulations, which may be used directly as sub-grid star formation models in global galaxy simulations.

Exploring streaming cosmic ray propagation in zoom-in molecular cloud simulations

Mon, 19 Aug 2024 00:00:00 +0000

Cosmic rays are charged, relativistic particles that pervade the galaxy at similar total energy densities as the magnetic fields and even the kinetic turbulent energies. The most common in number density are the GeV cosmic rays, which are subject to resonant instabilities with the magnetic fields embedded in the medium that they are propagating through. The net effect of the instability is to determine the dynamics of the distribution function, making populations of relativistic particles drift at the local ion Alfven speed. This tightly couples the distribution function to the dynamical timescales of the magnetic field, and subjects the particles to the structure and statistics that govern the ion Alfven fluctuations (the ionization state, the gas density, and the magnetic field). In this project we will explore how streaming GeV particles are transported through a host of different zoom-in simulations of molecular clouds. We will use the recently developed criptic code for doing post-processed cosmic ray transport, detailed in Krumholz et al. (2022), coupled with molecular cloud simulation data from global galaxy simulations detailed in Hu et al. (2023). We will investigate how the diverse morphology of the magnetic fields and ionization state of the gas in these systems gives rise to different diffusion coefficients, which can be compared directly with observations.

Growth or decay - decaying magnetohydrodynamics meets the turbulent dynamo

Mon, 19 Aug 2024 00:00:00 +0000

The saturation of the turbulent dynamo remains a highly important, outstanding problem for all small-scale dynamo theories. Beattie, et al. (2023a) showed numerically that the saturation is completely independent of the initial magnetic field conditions, even if the magnetic field decays into the saturation, which may be present in the post-shock region of supernova remnants. The decaying magnetic field presents a novel way of understanding dynamo saturation where the mechanisms for saturation are amplified due to the strong field. Preliminary analysis shows that the decaying field finds a force-free equilibrium state and that the decay is faster than Ohmic, potentially due to reconnection. In this project we will do a detailed analysis of the decay and force-free magnetic field in high-resolution 3D simulations of decaying plasma that are being constantly injected with momentum to stir weak turbulent modes. This will provide deep insights into the nature of dynamo saturation, and the stability of force-free magnetic fields, which are important for magnetisation in the early Universe and magnetic fields around compact objects.

Investigating compressible and incompressible mode coupling in supersonic turbulent dynamos relevant to the interstellar medium

Mon, 19 Aug 2024 00:00:00 +0000

The turbulent magnetic field that is grown and maintained in our Galaxy is roughly an order of magnitude larger in strength than the ordered magnetic field. The only way to keep such a field energised is through a turbulent dynamo. Classical turbulent dynamo theory takes no account of compressibility of the plasma, however the plasma in the interstellar medium of our Galaxy is weakly-compressible and mildy-supersonic on large scales (~100pc), and highly-compressible and highly-supersonic on smaller scales (~10pc). Hence, for understanding the turbulent dynamo in our Galaxy, we must consider supersonic dynamos. Supersonic dynamos are less efficient both in growth rate and the final saturated magnetic to kinetic energy ratio compared to incompressible dynamos. A good explanation for why has not yet been made nor proven from first principles, and in fact there is reason to believe that compressible modes should enhance the dynamo through compression. To explore this question, we will utilise an advanced compressible transfer function framework outlined in Grete et al. (2017), tracking the energy fluxes in high resolution simulations, mode by mode, for all terms in the compressible / incompressible mode decomposed magnetohydrodynamic fluid equations. In particular, we will develop a better understanding for how compressible modes couple to incompressible modes (and vice versa) on various scales in the dynamo, in turn determining how compressible modes potentially inhibit dynamo action and solving this outstanding problem in compressible dynamo theory.

Kinetic helicity and chiral velocity modes in supernova driven turbulence

Mon, 19 Aug 2024 00:00:00 +0000

There is sufficient energy in supernova detonations alone to drive the turbulence in our Galaxy. However, the nature of the supernova-driven cascade, the mechanism that transports energy from the largest scales to the smallest scales, is unknown for this kind of turbulence regime, where energy flux must travel both ways because the driving happens on small scales – from large to small in a direct cascade, and from small to large in an inverse cascade. It is well known that one inverse cascade mechanism is through interacting, incompressible homochiral modes (Plunian et al. 2020; i.e., velocity modes that generate vorticity with the same handedness). In this project, we will derive a new set of energy flux transfer functions for probing the interactions between the homochiral, heterochiral and compressible modes in a turbulent plasma. We will apply them directly to high resolution supernova-driven turbulence simulations to understand how the energy cascade works in the interstellar medium of our Galaxy.

Reconstructing three-dimensional moments from anisotropic two-dimensional fields

Mon, 19 Aug 2024 00:00:00 +0000

Many astrophysical observations are intrinsically two-dimensional in position-position space (PP; e.g., a column density map). However, astrophysical plasma models are usually constructed in three-dimensions, position-position-position (PPP), so an important step to compare theory to observations is therefore being able to reconstruct the statistics of the three dimensional field from two dimensional observations. Important work from Brunt et al. (2010) showed that one could, under the assumption of isotropy, reconstruct the three-dimensional variance of a turbulent (or generally stochastic) field by using a rotational transformation of the 2D power spectrum. But in the presence of strong magnetic fields, which we find on many scales in a galaxy, isotropy is strongly violated. Hence, this project aims to utilise analytical means to generalise the Brunt et al. (2010) method to include the ability to reconstruct anisotropic fields. Furthermore, we will validate our new method on a suite of high resolution magnetohydrodynamical turbulence simulations followed by applying them dust continuum emission observations of quiescent molecular clouds.

Supersonic vortices - understanding the building blocks of supersonic, sub-Alfvenic magnetohydrodynamic turbulence

Mon, 19 Aug 2024 00:00:00 +0000

Strongly magnetised, compressible turbulence is ubiquitous in the solar wind, atmosphere of compact objects, and even cold molecular and atomic gas distributed across the Galaxy. Beattie, et al. (2020b,2022a,2022c) has shown that in this regime of turbulence the energy budget is dominated not by turbulent nor Alfvenic fluctuations, as previously assumed, but rather rigid body vortices that are self-organised into a quasi-stationary state that give rise to non-classical dissipation, non-local intermittency effects, and peculiar decay characteristics that are currently not captured by any turbulence phenomenology. By utilising both computational and analytical techniques, in this project, we aim to (1) build a vortex tracking code to use on high-resolution, three-dimensional turbulence data, so that we can extract and characterise the local dynamics that give rise to, maintain, and eventually decay these vortices; and (2) explore the stability and signature of these vortices in linear eigenmode decompositions of the turbulent plasma. These results will have fundamental repercussions for not only strongly magnetised compressible turbulence theory (e.g., residual energy theory), but also for GeV cosmic ray transport, and the measurement of interstellar magnetic fields using Davis-Chandreshkar-Fermi methods.

The secret life of over-dense regions in interstellar turbulence

Mon, 19 Aug 2024 00:00:00 +0000

The initial conditions for star formation are embedded in the fractal gas density structures produced by supersonic, magnetised turbulence. We understand in a lot of detail relations between the global statistical properties and moments of the gas density field. However, we do not understand the local properties of the densest regions, which are just as, if not more important than the global properties, for understanding the star formation process. Roberston & Goldreich (2018) demonstrated how to identify, cluster and track in time over-dense regions by using a mixture of Lagrangian and Eulerian plasma statistics, unveiling a host of important properties of the dense regions in hydrodynamical turbulence. In this project we will do the same for magnetohydrodynamical turbulence, with the student contributing to a clustering and local statistical analysis code that has already been written by Dr. James Beattie. With some further software development, we will add time tracking, and the ability to generalise this code to other interesting structures in the magnetised turbulence, such as current sheets. There will also be opportunities to do an analytical analysis of the local statistical properties, such as the density profile, of the regions as the project progresses. This project will lead to significantly better understanding of not only the initial conditions for star formation, but also the role of strong gas density fluctuations in a magnetised, turbulent medium.

The transport and flux of magnetic helicity fluctuations

Mon, 19 Aug 2024 00:00:00 +0000

Magnetic helicity describes the topological knottedness of a magnetic field, and in ideal magnetohydrodynamics, it is an invariant. It plays an important role in large-scale dynamos, and the decay of primordial magnetic fields in the early Universe, due in part to net-helicity being associated with symmetry breaking, and the helicity directly changing the decay timescale. Recent works have shown that not only is magnetic helicity an invariant, but so is the magnetic helicity correlation function, making it an even more robust invariant than previously thought. In this project we will explore the nature of the magnetic helicity flux in MHD turbulence through the use of helicity flux transfer functions. We will derive the transfer functions from the helicity evolution equation, and apply them to high resolution MHD turbulence simulation, unravelling what mechanisms give rise to the well-known inverse helicity cascade, and in turn better understanding the role of MHD turbulence in transporting helicity where it can be utilised by large-scale dynamos.

🎉 10k simulation featured in the Leibniz Supercomputing Centre newsletter for July!

Mon, 08 Jul 2024 00:00:00 +0000

🎉 New Scientist features the 10k MHD simulation in print!

Sat, 08 Jun 2024 00:00:00 +0000

🎉Results from the world's largest MHD turbulence simulation hits the arXiv!

Wed, 29 May 2024 00:00:00 +0000

Magnetized compressible turbulence with a fluctuation dynamo and Reynolds numbers over a million

Wed, 29 May 2024 00:00:00 +0000

✈️I'm off to Tallahassee for the HEDLA meeting!

Mon, 20 May 2024 00:00:00 +0000

The Supersonic Turbulent Dynamo

Mon, 20 May 2024 00:00:00 +0000

Taking control of compressible modes: bulk viscosity and the turbulent dynamo

Mon, 01 Jan 2024 00:00:00 +0000

Experience

Tue, 24 Oct 2023 00:00:00 +0000

Growth or Decay - I: universality of the turbulent dynamo saturation

Fri, 01 Sep 2023 00:00:00 +0000

Turbulent diffusion of streaming cosmic rays in compressible, partially ionized plasma

Wed, 01 Feb 2023 00:00:00 +0000

The density distribution and physical origins of intermittency in supersonic, highly magnetized turbulence with diverse modes of driving

Thu, 01 Dec 2022 00:00:00 +0000

Availability, outage, and capacity of spatially correlated, Australasian free-space optical networks

Tue, 01 Nov 2022 00:00:00 +0000

Energy balance and Alfvén Mach numbers in compressible magnetohydrodynamic turbulence with a large-scale magnetic field

Sat, 01 Oct 2022 00:00:00 +0000

Magnetized compressible turbulence with a fluctuation dynamo and Reynolds numbers over a million

Sat, 01 Oct 2022 00:00:00 +0000

Fundamental scales in the kinematic phase of the turbulent dynamo

Fri, 01 Jul 2022 00:00:00 +0000

A multishock model for the density variance of anisotropic, highly magnetized, supersonic turbulence

Thu, 01 Jul 2021 00:00:00 +0000

The sonic scale of interstellar turbulence

Fri, 01 Jan 2021 00:00:00 +0000

Magnetic field fluctuations in anisotropic, supersonic turbulence

Thu, 01 Oct 2020 00:00:00 +0000

Filaments and striations: anisotropies in observed, supersonic, highly magnetized turbulent clouds

Sat, 01 Feb 2020 00:00:00 +0000

The relation between the turbulent Mach number and observed fractal dimensions of turbulent clouds

Sun, 01 Sep 2019 00:00:00 +0000

The relation between the true and observed fractal dimensions of turbulent clouds

Thu, 01 Aug 2019 00:00:00 +0000

Is The Starry Night Turbulent?

Fri, 01 Feb 2019 00:00:00 +0000

🎉Congrats Michael Grehan🎉 (CITA) -- student-led study submitted on magnetic reconnection through many different special relativistic plasma regimes!

Mon, 01 Jan 0001 00:00:00 +0000

Curriculum Vitae

Mon, 01 Jan 0001 00:00:00 +0000