Cosmic Rays Wander Between Clouds ✎ express

Original: "Diffusion of PeV Cosmic Rays in the Turbulent and Multiphase Interstellar Medium"
· Yue Hu
arXiv:2604.04814 · 2026-04-06 · arXiv non-exclusive · independent analysis · 1 min
Boundaries between warm and cold gas in the Galaxy act like mirrors, scattering particles.

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Interstellar space is not empty: it is filled with tenuous gas, which is warm in some places and cold in others. The boundaries between such regions resemble the walls between soap bubbles. When an ultra-energetic particle, a cosmic ray, hits such a wall, the magnetic field there changes abruptly, and the particle bounces off like a ball off a wall.

Scientists tracked millions of such particles in a computer model of the Galaxy. It turned out that cold, dense clouds act as traps: inside them, particles can barely move. But in the warm, tenuous medium, they glide freely along tangled magnetic field lines, like along winding paths. On average, this speeds up their journey through the Galaxy.

The fastest particles cross our Galaxy in tens of thousands of years — a blink of an eye by cosmic standards.

This picture helps us understand where particles with energies millions of times greater than those in the Large Hadron Collider come from. Perhaps their sources, exploded stars or black holes, are closer than previously thought.

A cosmic ray with an energy of 1 PeV carries as much energy as a tennis ball moving at 60 km/h, but packed into a single subatomic particle.

In the series "Star Trek," cosmic rays sometimes knock out ship systems — in reality, they do pose a threat to electronics and future interstellar flights.

Scientists
Enrico FermiFritz ZwickyTheodore LymanEmile ClapeyronJames JeansJohn Henry Poynting
Concepts
intracluster medium heat transport cosmic rays interstellar gas diffusion coefficient interstellar space galactic circumgalactic medium cosmic ray acceleration solar wind waves interplanetary magnetic field galactic winds energy transport wave propagation temperature gradient velocity distribution initial mass function coronal mass ejection hot gas star formation regions interstellar medium