A massive star doesn’t simply fade away — it blows up as a supernova, leaving behind an expanding remnant and a wildly spinning neutron star — a pulsar. In this cosmic storm, astonishing patterns emerge, and the 'Nimbus'–'Thunder' system is a dazzling illustration. The remnant looms like a raincloud, and piercing through it like lightning is a supersonic pulsar. Trailing behind is a three-parsec-long tail of emission — a bow shock frozen into the interstellar medium. Such bow-shock pulsar wind nebulae are rare, true windows into the lives of neutron stars on the brink of their journey.

Radio astronomy in full force: ASKAP and MeerKAT scrutinized the storm in detail, ATCA added a polarization map. The radio spectrum of 'Thunder' turned out flat (α ≈ −0.27) — the unmistakable signature of synchrotron glow from relativistic particles. The X-ray spectrum with a photon index of 1.6 confirmed: we’re looking at a genuine particle accelerator. And Faraday rotation maps — for the first time at this resolution — laid bare a magnetic tornado stretched along the pulsar’s motion.

The spectra of the pulsar wind nebula and the remnant (α ≈ −0.53) separated two acceleration mechanisms: the relativistic wind of the pulsar versus the classical Fermi acceleration at shock fronts. The system works as a natural collider for studying plasma and the birth of cosmic rays — particles with energies unattainable in Earthly laboratories.

'Thunder–Nimbus' is a snapshot of a late stage in the lives of neutron stars, as they leave the cradle and slam into the interstellar medium. In the future, the SKA will track the fate of particles in the tail, IXPE will probe the magnetic field geometry right at the surface of the pulsar, and CTA may see inverse Compton scattering. Such storms teach us to read the biographies of extreme objects — from solitary neutron stars to mergers that shake spacetime.