Beta Pictoris is a young, well-studied star system already known to host planets and a vast outer debris disk. New observations have provided a clearer look at the hot, fine dust orbiting very close to the star, known as exozodiacal dust. This material represents the fine, pulverized remains of collisions within the system and offers clues into the complex environment where planets and comets interact.
Using the MATISSE instrument at the Very Large Telescope Interferometer, researchers observed the star at infrared wavelengths of 3.5 microns. By developing new methods to account for data correlations, they were able to model the faint light emitted by this hot, inner dust. This technique allows for a precise measurement of the dust's location, shape, and grain composition.
The findings show a compact, highly inclined dust structure located just 0.05 astronomical units from the star, near the sublimation radius where temperatures are high enough to vaporize solid matter. This inner disk is misaligned by approximately 60 degrees relative to the star's large outer debris disk. The dust is composed of tiny, submicron-sized grains and contributes up to 7.5 percent of the system's total light at these wavelengths. There is also potential evidence for an additional dust population further out, near 1 astronomical unit.
Key findings
- Detection of a compact dust structure located 0.05 astronomical units from Beta Pictoris.
- The inner dust disk is misaligned by 60 degrees compared to the main outer debris disk.
- Dust is composed of submicron-sized grains near the sublimation radius.
- The inner dust contributes 4 to 7.5 percent of the system's total flux at 3.4 microns.
- Data support a potential additional dust component located near 1 astronomical unit.
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25. 9. 2026
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