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Black holes do not launch powerful jets on a universal countdown. A 2026 Nature Astronomy study finds that a delayed outflow begins when feeding falls to about 0.02 of the Eddington limit—roughly 2% of the maximum rate at which radiation pressure can balance gravity. In tidal-disruption events, that transition can occur hundreds or thousands of days after a star is torn apart, explaining why some black holes appear dormant before suddenly producing a radio-bright outflow.
What triggers a delayed black-hole jet?
The trigger is an accretion-state change, not the passage of a fixed number of days. When a supermassive black hole shreds a star, the debris returns toward the black hole at a rate that changes over time. The initial feeding episode can be super-Eddington, meaning the inflow is above the Eddington scale. As the debris supply declines, the accretion rate eventually reaches approximately 0.02 LEdd. The study identifies that threshold as the point at which a second, physically distinct outflow can appear.
Because the debris settles and drains at different rates in different events, the threshold may be reached quickly in one tidal-disruption event (TDE) and much later in another. “Thousands of days” therefore describes an observed TDE timescale, not a universal waiting period that applies to every black hole.
The two outflow phases
| Feature | Early outflow | Delayed outflow |
|---|---|---|
| Accretion regime | Super-Eddington feeding | Approximately 0.02 of the Eddington limit |
| Timing after stellar disruption | Prompt, during the early feeding episode | Hundreds to thousands of days, depending on debris evolution |
| Observed signature | Early outflow associated with the disruption | Later radio outflow or jet-like activity |
| Physical interpretation | Outflow produced in the high-rate accretion state | Outflow launched after a transition to a lower-rate state |
The distinction matters because a late radio signal is not simply a delayed echo of the first event. It marks a separate outflow phase associated with the accretion flow crossing the critical rate.
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How astronomers could see a process that normally takes millennia
Supermassive black holes evolve too slowly for observers to watch their full feeding cycles directly. TDEs provide a natural time-lapse experiment: a star is disrupted, and the resulting debris feeds the black hole over a period of years rather than the much longer timescales typical of ordinary supermassive-black-hole growth.
The team first assembled 20 TDEs and then selected 10 high-quality events with enough multi-wavelength observations to model both the feeding rate and the timing of radio outflows. Combining those measurements allowed the investigators to compare when the accretion rate crossed the proposed threshold with when late radio activity appeared.
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- Identify a TDE: observe the flare produced when a star is torn apart by a supermassive black hole.
- Track the feeding episode: use observations across multiple wavelengths to estimate how the debris supply and accretion rate change.
- Monitor for outflows: continue radio observations after the initial flare rather than stopping once the prompt emission fades.
- Compare timing: test whether a later outflow appears as the modeled rate approaches about 2% of the Eddington limit.
Why the 2% threshold is important
Stellar-mass black holes are already known to change jet behavior near a similar fraction of the Eddington rate. Finding approximately the same transition point in supermassive black holes supports a scale-invariant accretion–outflow process: the underlying state change may operate in the same way even when the black hole masses differ by millions or billions of times.
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What observers should do differently
A TDE that shows no immediate jet should not be classified as permanently inactive. The late phase may emerge only after the debris supply has declined substantially. The Institute for Advanced Study account of the study highlights a practical consequence: sustained radio monitoring can reveal outflows that a short observing campaign would miss.
A Space.com report recommends a two-to-six-year follow-up window for searching for late radio signals. That interval is an observing recommendation, not a universal law from the Nature Astronomy paper. Actual scheduling should be guided by the event’s measured light curve and estimated accretion rate, with radio observations concentrated as the system approaches the critical state.
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What the finding does—and does not—prove
- Established by the study: a delayed outflow is associated with accretion declining to about 0.02 of the Eddington limit in the modeled TDE sample.
- Supported interpretation: the late outflow is a distinct low-rate accretion-state transition rather than a timer set at disruption.
- Broader implication: a common jet-launching rule may span stellar-mass and supermassive black holes.
- Not established: an exact launch day for every TDE, a guarantee that every supermassive black hole will produce a detectable jet, or identical jet power across events.
The sample is deliberately selective: 10 of the 20 identified TDEs had sufficiently complete data for the detailed modeling. More events with long-term, multi-wavelength coverage will be needed to determine how often the predicted transition produces a detectable radio jet and how its strength varies.
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Jet searches have traditionally favored the dramatic moment immediately after a disruption. The threshold result adds a second strategy: estimate the declining accretion rate, then reserve radio and other telescope time for the period when the system approaches 2% of Eddington. That approach could make scarce observing time more efficient and help explain why otherwise similar TDEs have very different radio histories.
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As Adelle Goodwin told the Institute for Advanced Study, “When a black hole tears apart a star, it does not swallow everything neatly.” Some debris can remain in orbit, settle gradually, and feed the black hole through changing accretion states. Andrew Mummery framed the puzzle as why some black holes launch radio jets immediately while others remain quiet for months or years. The new model connects both outcomes to where the system is on its accretion-rate track.
The practical takeaway
A black hole can wait years to launch a jet because the relevant clock is the decline of its fuel supply. Once the accretion rate falls from the initial super-Eddington phase to roughly 2% of the Eddington limit, a second outflow may be triggered. In TDEs, that physical transition can take hundreds or thousands of days, so long-term radio monitoring is essential for catching the event.
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