What travels almost one-fifth the velocity of light and erupts from the heart of a galaxy? For the very first time, astronomers have just watched it happen-the birth of an ultrafast outflow, or “UFO,” from a supermassive black hole. This remarkable event, traveling at 57,000 kilometers per second, offers the first-ever look at the extreme process in which black holes can fling matter back into space with tremendous force.
The phenomenon unfolded in NGC 3783, a barred spiral galaxy about 135 million light-years away in the constellation Centaurus. There, a black hole of roughly 2.8 million solar masses lies at the center, enveloped by a turbulent accretion disk in the form of a swirling maelstrom of gas and dust spiraling toward the event horizon. Scientists observed a sudden flare in X-ray light, followed by the rapid emergence of the high-speed wind during a continuous 10-day observation campaign using ESA’s XMM-Newton and JAXA’s XRISM space telescopes. “For the first time, we’ve seen how a rapid burst of X-ray light from a black hole immediately triggers ultra-fast winds, with these winds forming in just a single day.” said Dr. Liyi Gu of the Space Research Organisation Netherlands.
It was a question of timing. Within roughly 12 hours of the flare’s onset, the telescopes recorded spectral signatures of highly ionized gas racing outward at relativistic speeds. The most plausible trigger is magnetic reconnection a sudden reconfiguration of magnetic field lines in the accretion disk, releasing huge amounts of energy. This process is the same physics as involved in solar flares and coronal mass ejections, but billions of times more powerful. On the Sun, magnetic reconnection hurls hot plasma into space; on the black hole of NGC 3783, it expelled matter from a region roughly 50 times the black hole’s own size.
The mechanics of such outflows are rooted in magnetohydrodynamics-the science of how magnetic fields interact with ionized gases. In the relativistic regime near a black hole, MHD becomes even more complex, since warped spacetime and gravity itself influence plasma motion. Large-scale magnetic fields threading an accretion disk can accelerate particles along field lines; this process is, moreover, enhanced when rotation twists those lines into powerful toroidal structures. Such configurations, as recent GRMHD models show, can launch winds at speeds from 0.03c to 0.3c-appropriately matching the measured velocities of UFOs.
These are not mere curiosities-these are “feedback” winds that can reshape galaxies. Black holes can control star birth by blowing mass and energy out of a galaxy, disperse interstellar gas, and participate in the chemical evolution around them. Among AGN, these ultrafast outflows have been detected (most often by the blueshifted X-ray absorption lines from iron ions) in as many as half of observed systems. The event in NGC 3783 represents the first time astronomers have witnessed the launch, and thus directly linked it to the flare.
It was a question of instrumentation: the high-resolution spectroscopy of XRISM followed changes in X-ray brightness and energy distribution in great detail; at the same time, XMM-Newton provided the continuous coverage needed to capture the flare through its full evolution. Together, they could pinpoint the sequence: first, a spike in hard X-rays; then, a peak in softer X-rays; finally, the acceleration phase of the wind. This synergy of observatories is similar to the multi-wavelength approach taken while studying relativistic jets, where radio, optical, and gamma-ray data are combined to discern the physics of particle acceleration.
The parallels with jet formation are striking: in all cases, magnetic fields and rotation are the key drivers. The wellknown Blandford–Znajek mechanism describes how a spinning black hole’s rotational energy can be tapped via magnetic fields to power jets. In this case, in the NGC 3783 UFO, magnetic reconnection seems to have provided the energy burst necessary for the material to break out of the gravitational clutches and be thrown outwards. Numerical simulations, such as those using the Frankfurt Particle-In-Cell code, illustrate how reconnection can produce plasmoids compact blobs of plasma that travel at relativistic speeds and could account for the structure observed in this wind.
For the astrophysicists, this is a goldmine. It serves as a direct test for theories of the dynamics of an accretion disk, the evolution of magnetic fields, and the acceleration of high-energy particles. It also reaches across scales: from solar eruptions in our immediate system to galaxy-shaping winds in the distant universe.
As ESA’s Erik Kuulkers noted, “Excitingly, this suggests that solar and high-energy physics may work in surprisingly familiar ways throughout the Universe.” Future missions will seek to capture even more of these cosmic blasts in real time, refining the models of how black holes consume and expel matter. With each observation, the picture sharpens: black holes are not just voracious cosmic sinks but also engines capable of launching some of the fastest winds ever seen.
