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Sky Hotspots: The Senders of Ultra-Particles Identified ⚡ экспресс

Original: "Rare Transients in Nearby Galaxies Explain Ultra-high-energy Cosmic Rays"
· Imre Bartos, Marek Kowalski
arXiv:2510.06193 · 2025-10-07 · CC BY 4.0 · ⏱ 1 min · High Energy
Neutron star mergers in nearby galaxies explain the clumps of cosmic rays in the sky.
Abstract

Cosmic rays are particles with enormous energy, flying in from the depths of the universe. Scientists have discovered that their sources are likely in nearby galaxies, where neutron stars collide. It's like tracing footsteps back to specific houses on our cosmic street. Could our stellar neighbors really be the accelerators?

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Every day, particles with colossal energy enter Earth's atmosphere—like unsigned letters. Their source long remained a mystery. New research shows: these 'visitors' point to nearby galaxies, where from time to time catastrophes occur—collisions of neutron stars, ultra-dense spheres the size of a city but with the mass of the Sun. Upon impact, they scatter particles like postal items, and some fly straight to us.

Seven of the ten brightest nearby galaxies precisely coincide with hotspots in the sky where particles are especially abundant. The chance of such a coincidence happening randomly is less than one-tenth of a percent.

The same model explains why the northern and southern hemispheres see a slightly different 'assortment' of particles: simply, the nearest 'post offices'—the sources—are located on different sides of the sky. Previously, it was thought that the composition of rays depends only on energy, but now it's clear: the key to the puzzle lies in the arrangement of the sender galaxies.

🎯 One such particle, smaller than an atom, carries energy comparable to a baseball's impact—like a carrier pigeon delivering a truck.

Scientists
Enrico FermiPaul DiracFritz ZwickySubrahmanyan ChandrasekharAugustin-Louis CauchyChristiaan Huygens
Tags
neutron star galaxy supernova
Laws
Fermi–Dirac statisticsvirial theoremChandrasekhar limitFermi accelerationlaw of conservation of momentumquadrupole radiation formula
Original: arXiv:2510.06193 · CC BY 4.0 · bridge42worlds