Well, could the same magnetic chaos that powers solar flares also drive some of the universe’s fastest winds? Astronomers have just watched a supermassive black hole perform something startlingly familiar-but on a scale billions of times more extreme.
At the centre of the spiral galaxy NGC 3783, about 130 million light-years from Earth, lies a black hole with a mass of approximately 30 million Suns. Thanks to a ten‑day campaign led by the XRISM X‑ray space telescope, and with supporting observations from ESA’s XMM‑Newton, researchers caught this cosmic giant in the act of producing a flare of X‑ray light so intense it triggered an ultrafast outflow of matter. Within hours, a gale of hot, ionized gas erupted from the accretion disk-the swirling plasma feeding the black hole-blasting outward at 57,000 km/s, or about 20% of the speed of light.
The precision of the Resolve microcalorimeter on XRISM allowed scientists to resolve narrow absorption lines from highly ionized iron and unveil a velocity dispersion of the outflow of around 1,000 km/s. The data showed the wind originated from a dense clump located around 50 times the radius of the black hole, in a region where the forces of gravity and magnetic fields wrestle for dominance. It was not possible for radiation pressure to accelerate the wind so quickly. Instead, the kinematic evolution fitted the profile of a solar coronal mass ejection, with magnetic reconnection the snapping and re‑joining of magnetic field lines-being the likely launch mechanism.
Magnetic reconnection is well known in heliophysics, where it drives solar flares and sends huge clouds of plasma into the solar system. Near a supermassive black hole, this process takes place within an environment of far stronger fields and deeper gravitational wells. Numerical simulations, like those using the Frankfurt particle‑in‑cell code for black hole spacetimes, have demonstrated that reconnection in the equatorial plane can create chains of plasmoids—magnetically confined plasma bubbles—that are accelerated to relativistic speeds. These events can tap into the black hole’s rotational energy, adding to the explosive output.
The flare in NGC 3783 was short-lived, but its effect was dramatic. This magnetic field untwisted similarly to the coronal mass ejections of the Sun, flinging plasma into space, but here the eruption was ten billion times more powerful. In terms of its kinetic energy, this wind is classified in the class of UFOs: ultrafast outflows, phenomena capable of influencing galaxy-scale evolution. With column densities around 10²³ cm⁻², such winds can carry mechanical energies exceeding several percent of the black hole’s bolometric luminosity-enough to expel interstellar gas, quench star formation, and regulate the growth of the galactic bulge.
There were also hints of further, slower components. A transient outflow at 3,700 km/s seemed to cover the Fe Kβ emission line during the flare decay phase, implying a multi‑layered wind structure. This is in accord with hydrodynamic and radiative transfer models of the outflows from AGN which predict that the dense gas is fragmented into polar funnels and embedded in far more tenuous streams. Such structures do arise in high-resolution simulations where radiation pressure and centrifugal forces act together to destabilize infalling material, causing clumping into denser clouds with variable absorption signatures.
From a feedback perspective, the event offers a rare, time‑resolved view of how energy and momentum are injected into a galaxy’s interstellar medium. Relativistic jet feedback studies show that mechanical power input in the range of 10⁴³–10⁴⁶ erg/s can disperse dense, star‑forming clouds within a kiloparsec of the core. The NGC 3783 wind was not a sustained jet, but its speed and density suggest it might deliver similar disruptions on smaller scales. The porosity of the surrounding medium—how patchy or clumpy the gas is—will determine whether an outflow like this one escapes into the galaxy or stalls, compressing clouds and potentially triggering new star formation.
The statistical significance of the detection was further strengthened by cross-checks with XMM-Newton, NuSTAR, and XRISM’s Xtend imager, with combined analysis reducing the probability of a random feature to just 3 × 10⁻⁷. This level of confidence, added to the temporal link between flare and wind, makes the case for magnetic-driven acceleration compelling. It also bridges solar and high-energy astrophysics, showing that the same physical principles shaping space weather in our solar system can operate in the extreme environment near a black hole’s event horizon-only vastly amplified.
