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1Fix the driver behind crashes, sound loss and screen glitches2Clear out junk files and repair common Windows errors3Scan for outdated or missing drivers - takes under a minuteRoughly 1% of young stars show observable signs of an unusually violent stage of planet formation: an extreme debris disk, where abundant warm dust near the star appears to be generated by collisions among rocky planetary building blocks. That figure is an estimate from systems observed so far—not proof that only 1% of young stars ever undergo such collisions. NASA and ESA report that Webb’s infrared observations are helping researchers read the dust left behind, rather than directly watch the impacts happen.
What is the violent phase around young stars?
An extreme debris disk is a warm, dusty belt close to a star, in the region where rocky planets form. Its unusually abundant dust and changing infrared brightness are interpreted as signs of ongoing or recent collisions between planetary embryos—the small bodies that can eventually combine into planets.
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It is not the same as a gas-rich protoplanetary disk around a very young star, nor a typical cold debris disk such as those around Vega or Fomalhaut. Extreme debris disks are distinguished by concentrated warm dust and unusually small grains. The evidence points to violence in the system, but the collisions themselves have not been directly imaged.
What did Webb reveal about the dust?
NASA and ESA describe a compiled sample of 21 extreme debris disks: five identified from Spitzer archival data and 16 observed with Webb. The Webb portion includes 12 newly observed disks and follow-up observations of four systems previously studied by Spitzer. By examining mid-infrared emission and spectral features, the team identified mineral components in the dust.
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The grains are described as predominantly smaller than a micrometre and thermally altered. Silica and crystalline silicates appear among the identified materials. These signatures give researchers clues to the conditions under which the dust formed: intense impacts can heat and alter rocky material, sometimes vaporizing part of it.
Two dust signatures point to different collision scales
About one-third of the disks in the sample are silica-rich; the remaining two-thirds are silica-poor. Researchers interpret that contrast as evidence for different kinds of impacts. The collision scale is an inference from dust composition and other observed properties, not a direct measurement of the bodies involved.
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| Observed group | Dust signature | Researchers’ interpretation | Age and variability reported |
|---|---|---|---|
| Silica-rich, about one-third of the sample | Relatively abundant silica, consistent with material that experienced very high temperatures | High-energy collisions between Mars-sized bodies, with some material vaporized | Observed only around stars younger than 300 million years in this sample |
| Silica-poor, about two-thirds of the sample | Less silica | Smaller-scale impacts, sometimes grazing collisions, involving Moon-sized bodies | Appears across a wider range of stellar ages; these disks often show greater infrared brightness variability |
The brightness changes are another measured clue. The team proposes that rapid changes in orbits and additional impacts could help explain the variability, especially in silica-poor systems. That is a proposed explanation, not a filmed sequence of events.
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The roughly 1% figure refers to young stars with observable signatures of extreme debris disks in data collected so far, as reported by the NASA Webb Mission Team and ESA/Webb in 2026. It is not a definitive count of every young star, a lifetime probability, or a measure of how long the phase lasts. A short-lived or difficult-to-detect phase could be missed in a snapshot of the sky.
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Age comparisons also need care. Silica-rich disks in this sample occur only around stars younger than 300 million years, but the sample contains just three disks older than that threshold. The small number limits how strongly researchers can conclude that older silica-rich systems do not exist; the team says more observations are needed.
Independent reader supportYour contribution helps us test, update, and keep practical guides available for everyone.What this could mean for our solar system
The findings offer a way to compare other planetary systems with possible episodes in our own solar system’s past, including the impact thought to have formed the Moon and a possible later period of dynamical instability. Webb did not observe the early solar system. Rather, the dust around distant stars may preserve clues to processes that planetary systems—including ours—could experience while forming and evolving.
Quick Recap
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- UNASSEMBLED HOBBY MODEL KIT – packed in an envelope with easy to follow instructions. Ideal for ages 14 and up.
- NO GLUE OR SOLDER NEEDED – Parts can be easily clipped from the metal sheets. Bundle includes tweezers, which are recommended for bending and twisting the connection tabs.
- JAMES WEBB SPACE TELESCOPE - 2.75 Sheet Model with a moderate difficulty level. Assembled Size: 4.13 L x 2.75 W x 2.75 H inches. 1:221 Scale. 62 Pieces.
- FROM STEEL SHEETS TO 3D – Pop out the pieces and connect using tabs and holes. Includes illustrated instructions.
- HIGHLY DETAILED ETCHED MODEL – Display your 3D model once completed - collect and build them all.
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