Astrophysicists explore our galaxy’s magnetic turbulence in unprecedented detail using a new computer model

Astronomers have developed a computer simulation to explore, in unprecedented detail, magnetism and turbulence in the interstellar medium (ISM)—the vast ocean of gas and charged particles that lies between stars in the Milky Way galaxy.

Described in a study published in Nature Astronomy, the model is the most powerful to date, requiring the computing capability of the SuperMUC-NG supercomputer at the Leibniz Supercomputing Center in Germany. It directly challenges our understanding of how magnetized turbulence operates in astrophysical environments.

James Beattie, the paper’s lead author and a postdoctoral researcher at the Canadian Institute for Theoretical Astrophysics (CITA) at the University of Toronto, is hopeful the model will provide new insights into the ISM, the magnetism of the Milky Way galaxy as a whole, and astrophysical phenomena such as star formation and the propagation of cosmic rays.

“This is the first time we can study these phenomena at this level of precision and at these different scales,” he says.

The paper was co-authored with researchers from Princeton University; Australian National University; the Australian Research Council Center of Excellence in All Sky Astrophysics; Universität Heidelberg; the Center for Astrophysics, Harvard & Smithsonian; Harvard University; and the Bavarian Academy of Sciences and Humanities.

“Turbulence remains one of the greatest unsolved problems in classical mechanics,” says Beattie, who also holds a joint appointment at Princeton University. “This despite the fact that turbulence is ubiquitous: from swirling milk in our coffee to chaotic flows in the oceans, solar wind, interstellar medium, even the plasma between galaxies.

“The key distinction in astrophysical environments is the presence of magnetic fields, which fundamentally alter the nature of turbulent flows.”

While there are far, far fewer particles in interstellar space than in ultra-high vacuum experiments on Earth, their motions are enough to generate a magnetic field, not unlike how the motion of our planet’s molten core generates Earth’s magnetic field.

And while the galactic magnetic field is a few million times weaker than a fridge magnet, it is nonetheless one of the forces that shapes the cosmos.

The largest version of Beattie’s model is a cube of 10,000 units per dimension that provides much greater detail than previous models. In addition to its high resolution, the model is scalable and can simulate, at its largest, a volume of space some 30 light-years on a side; at its smallest, it can be scaled down by a factor of some 5,000.

At its largest, the model can improve our understanding of the Milky Way galaxy’s overall magnetic field. When scaled down, it will help astronomers better understand more “compact” processes like the solar wind that streams outward from the sun and greatly affects Earth.

Because of its higher resolution, the model also has the potential to provide a deeper understanding of star formation. “We know that magnetic pressure opposes star formation by pushing outward against gravity as it tries to collapse a star-forming nebula,” says Beattie. “Now we can quantify in detail what to expect from magnetic turbulence on those kinds of scales.”

In addition to its higher resolution and scalability, the model also marks a significant advance by simulating the dynamic changes in the density of the ISM—from an incredibly tenuous near-vacuum to the higher densities found in star-forming nebulas.

“What our simulation captures really well,” says Beattie, “is the extreme changes in density of the ISM, something previous models hadn’t taken into account.”

As he develops the next generation of the model with, among other features, even higher resolution, Beattie is also testing his simulation against data collected from observations of the sun-Earth system.

“We’ve already begun testing whether the model matches existing data from the solar wind and Earth—and it’s looking very good,” says Beattie.

“This is very exciting because it means we can learn about space weather with our simulation. Space weather is very important because we’re talking about the charged particles that bombard satellites and humans in space and have other terrestrial effects.”

According to Beattie, the new model comes at a time of growing interest in astrophysical turbulence, as well as burgeoning observations of the ISM. And as new instruments such as the Square Kilometer Array (SKA) come online—with the ability to measure fluctuations in turbulent magnetic fields across the galaxy in great detail—accurate theoretical frameworks like his for interpreting magnetic turbulence will become even more critical.

One of the things that draws Beattie to this research is its elegant consistency—from intergalactic plasma to the swirl in a cup of coffee.

“I love doing turbulence research because of its universality,” says Beattie. “It looks the same whether you’re looking at the plasma between galaxies, within galaxies, within the solar system, in a cup of coffee or in Van Gogh’s The Starry Night.

“There’s something very romantic about how it appears at all these different levels and I think that’s very exciting.”