For the first time, astronomers watched a supermassive black hole launch an ultra-fast wind within a day of an X-ray flare — revealing how magnetism may power galaxy-shaping winds.
Astronomers have witnessed something unprecedented: a supermassive black hole in NGC 3783 triggered an ultra-fast wind within hours of an X-ray flare — all caught on camera by ESA’s XMM-Newton and JAXA’s XRISM. This isn’t just another observation; it’s a direct link between flare activity and wind generation, proving magnetic forces may be the engine behind these cosmic jets.
The black hole, weighing nearly 30 million solar masses, resides in an active galactic nucleus — a powerhouse where gas and dust spiral inward before being blasted outward as winds. Previous studies struggled to pinpoint exactly when or how these winds form because they’re fleeting and require high-resolution instruments. This event changed that.
Researchers led by Liyi Gu of SRON observed the flare over a 10-day campaign in late July 2024. They tracked rapid changes across soft and hard X-ray bands, identifying a unique “soft flare” phase during which the black hole emitted intense radiation. Within days, they detected a wind racing outward at 60,000 kilometers per second — roughly one-fifth the speed of light.
This is extraordinary. “We’ve not watched a black hole create winds this speedily before,” Gu said. “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.”
The key insight came from analyzing spectral data. During the flare’s decay phase, XRISM’s Resolve instrument detected an absorption dip near 8.4 keV — a signature of extremely ionized iron. Adding a photoionized absorber model improved the fit dramatically, revealing a wind speed of 56,780 ± 450 km/s — faster than any previously measured in real time.
“Other telescopes in the campaign had lower spectral resolution, but they still supported the signal,” Gu explained. “When our team added the same absorber to data from XRISM’s Xtend detector, XMM-Newton, and NuSTAR, the combined improvement remained significant. We also ran extensive simulations to account for random features — after correction, we reported a very low probability of false detection.”
What makes this even more remarkable is the timescale. The wind appeared within the same observing run that captured the flare — essentially real-time physics. This allows researchers to test causal links between events, something impossible with averaged spectra.
Why Magnetism Looks Like the Culprit
The mechanism driving ultra-fast outflows remains debated — heat, radiation, or magnetic fields? In many AGNs with modest accretion rates, radiation struggles to push ionized gas efficiently through line driving. That leaves magnetic forces as a prime candidate.
Guainazzi, XRISM Project Scientist, likened the phenomenon to solar coronal mass ejections: “The winds around this black hole seem to have been created as the AGN’s tangled magnetic field suddenly ‘untwisted’ — similar to the flares that erupt from the sun, but on a scale almost too big to imagine.”
The timing supports a two-stage process: a slow rise followed by fast acceleration — mirroring solar flares. A modest UV increase noted after the soft X-ray peak further suggests a broader disturbance in the system.
The team also discovered a second, slower wind moving at about 3,720 ± 480 km/s — faster than typical “warm absorbers” but far slower than the ultra-fast outflow. This suggests layered gas structures crossing the line of sight — a messy environment where multiple components interact.
Column density jumped during the decay phase, hinting at denser pockets of gas moving across the view. While the covering factor is uncertain, the true density could be higher than initial models suggest — meaning these winds might carry more momentum than previously thought.
Implications for Galaxy Evolution
Ultra-fast outflows aren’t just cosmic fireworks — they’re crucial to how galaxies evolve. Known as “AGN feedback,” these winds can heat or eject star-forming gas, shutting down new star birth. Understanding their mechanics helps explain why some galaxies remain quiescent while others churn with stars.
“Windy AGNs also play a big role in how their host galaxies evolve over time, and how they form new stars,” said Camille Diez, an ESA Research Fellow. “Because they’re so influential, knowing more about the magnetism of AGNs, and how they whip up winds such as these, is key to understanding the history of galaxies throughout the universe.”
This discovery provides a roadmap for future research. As XRISM and XMM-Newton continue coordinated monitoring, scientists expect more “cause and effect” cases like this one — allowing precise measurements of wind speed, density, and geometry. These will sharpen estimates of momentum and energy carried away — essential for modeling galaxy evolution.
The findings were published in Astronomy & Astrophysics. Researchers emphasize this is only the beginning — future observations promise deeper insights into how magnetism powers cosmic winds and shapes galaxies across time.
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