151 citations · 490 across the 28 of their papers we have counts for
21 papers · 1 filter
From IFS Maps to 3D Structure I: Constraining Geometry in the Circumgalactic Medium
Mandy C. Chen, Michael Rauch, Zhijie Qu +3
The three-dimensional geometric structure of the cool (T~ K) circumgalactic medium (CGM) -- the line-of-sight depth and the number of discrete clumps -- is poorly constrained…
What is the Strouhal number of turbulence driven by supernovae?
James R. Beattie, Isabelle Connor, Enrico Ramirez-Ruiz
The Strouhal number, , measures the temporal coherence of turbulent driving relative to the outer-scale eddy turnover time. In turbulence-box mod…
Cosmic ray and plasma coupling for isothermal supersonic turbulence in the magnetized interstellar medium
Matt L. Sampson, James R. Beattie, Romain Teyssier +5
Cosmic rays (CRs) are an integral part of the non-thermal pressure budget in the interstellar medium (ISM) and are the leading-order ionization mechanism in cold molecular clouds.…
The spectrum of magnetized turbulence in the interstellar medium
James R. Beattie, Christoph Federrath, Ralf S. Klessen +2
The interstellar medium (ISM) of our Galaxy is magnetized, compressible and turbulent, influencing many key ISM properties, like star formation, cosmic ray transport, and metal and…
So long Kolmogorov: the forward and backward turbulence cascades in a supernovae-driven, multiphase interstellar medium
James R. Beattie, Anne Noer Kolborg, Enrico Ramirez-Ruiz +1
The interstellar medium (ISM) of disk galaxies is turbulent, and yet the fundamental nature of ISM turbulence, the energy cascade, is not understood in detail. In this study, we us…
Magnetized compressible turbulence with a fluctuation dynamo and Reynolds numbers over a million
James R. Beattie, Christoph Federrath, Ralf S. Klessen +2
Supersonic magnetohydrodynamic (MHD) turbulence is a ubiquitous state for many astrophysical plasmas. However, even the basic statistics for this type of turbulence remains uncerta…
Taking control of compressible modes: bulk viscosity and the turbulent dynamo
James R. Beattie, Christoph Federrath, Neco Kriel +2
Many polyatomic astrophysical plasmas are compressible and out of chemical and thermal equilibrium, introducing a bulk viscosity into the plasma via the internal degrees of freedom…
Fundamental MHD scales -- II: the kinematic phase of the supersonic small-scale dynamo
Neco Kriel, James R. Beattie, Christoph Federrath +2
Many astrophysical small-scale dynamos (SSDs) amplify weak magnetic fields via highly compressible, supersonic turbulence, but established SSD theories have overlooked these compre…
Growth or Decay -- I: universality of the turbulent dynamo saturation
James R. Beattie, Christoph Federrath, Neco Kriel +2
The turbulent small-scale dynamo (SSD) is likely to be responsible for the magnetisation of the interstellar medium (ISM) that we observe in the Universe today. The SSD efficiently…
Turbulent diffusion of streaming cosmic rays in compressible, partially ionised plasma
Matt L. Sampson, James R. Beattie, Mark R. Krumholz +3
Cosmic rays (CRs) are a dynamically important component of the interstellar medium (ISM) of galaxies. The GeV CRs that carry most CR energy and pressure are likely confined b…
Ion Alfvén velocity fluctuations and implications for the diffusion of streaming cosmic rays
James R. Beattie, Mark R. Krumholz, Christoph Federrath +2
The interstellar medium (ISM) of star-forming galaxies is magnetized and turbulent. Cosmic rays (CRs) propagate through it, and those with energies from …
Energy balance and Alfvén Mach numbers in compressible magnetohydrodynamic turbulence with a large-scale magnetic field
James R. Beattie, Mark R. Krumholz, Raphael Skalidis +5
Energy equipartition is a powerful theoretical tool for understanding astrophysical plasmas. It is invoked, for example, to measure magnetic fields in the interstellar medium (ISM)…
First extragalactic measurement of the turbulence driving parameter: ALMA observations of the star-forming region N159E in the Large Magellanic Cloud
Piyush Sharda, Shyam H. Menon, Christoph Federrath +13
Studying the driving modes of turbulence is important for characterizing the impact of turbulence in various astrophysical environments. The driving mode of turbulence is parameter…
Why take the square root? An assessment of interstellar magnetic field strength estimation methods
R. Skalidis, J. Sternberg, J. R. Beattie +2
The magnetic field strength in interstellar clouds can be estimated indirectly by using the spread of dust polarization angles (). The method developed by Davis 1951 and by Cha…
The density distribution and physical origins of intermittency in supersonic, highly magnetised turbulence with diverse modes of driving
James R. Beattie, Philip Mocz, Christoph Federrath +1
The probability density function (PDF) of the logarithmic density contrast, , with gas density and mean density , for hydrodynamical supersonic turbulence i…
A multi-shock model for the density variance of anisotropic, highly-magnetised, supersonic turbulence
James R. Beattie, Philip Mocz, Christoph Federrath +1
Shocks form the basis of our understanding for the density and velocity statistics of supersonic turbulent flows, such as those found in the cool interstellar medium (ISM). The var…
The sonic scale revealed by the world's largest supersonic turbulence simulation
Christoph Federrath, Ralf S. Klessen, Luigi Iapichino +1
Understanding the physics of turbulence is crucial for many applications, including weather, industry, and astrophysics. In the interstellar medium (ISM), supersonic turbulence pla…
Magnetic field fluctuations in anisotropic, supersonic turbulence
James R. Beattie, Christoph Federrath, Amit Seta
The rich structure that we observe in molecular clouds is due to the interplay between strong magnetic fields and supersonic (turbulent) velocity fluctuations. The velocity fluctua…
Filaments and striations: anisotropies in observed, supersonic, highly-magnetised turbulent clouds
James R. Beattie, Christoph Federrath
Stars form in highly-magnetised, supersonic turbulent molecular clouds. Many of the tools and models that we use to carry out star formation studies rely upon the assumption of clo…
The relation between the turbulent Mach number and observed fractal dimensions of turbulent clouds
James R. Beattie, Christoph Federrath, Ralf S. Klessen +1
Supersonic turbulence is a key player in controlling the structure and star formation potential of molecular clouds (MCs). The three-dimensional (3D) turbulent Mach number, $\mathc…
The relation between the true and observed fractal dimensions of turbulent clouds
James R. Beattie, Christoph Federrath, Ralf S. Klessen
Observations of interstellar gas clouds are typically limited to two-dimensional (2D) projections of the intrinsically three-dimensional (3D) structure of the clouds. In this study…