High resolution imaging reveals double-peaked dust structure in the TW Hydrae disk

The TW Hydrae protoplanetary disk, a swirling cloud of gas and dust surrounding a young star where planets are currently forming, contains a prominent localized accumulation of dust located at a distance of 52 astronomical units from the star. New observations provide a high-resolution look at the internal structure and movement of this feature, which is commonly referred to as a dust blob. The study clarifies how this material moves and its possible nature within the disk.

By comparing high-resolution data from 2021 with archival observations taken in 2017, the motion of the dust blob was measured. It moves at an azimuthal speed of approximately 3.3 kilometers per second, which aligns with Keplerian rotation, the standard orbital motion expected for material within a disk. The structure is confirmed to be moving along with the rest of the disk system without significant inward or outward migration.

Advanced image reconstruction reveals that the dust blob is not a single mass, but possesses a distinct double-peaked shape separated by 1.7 astronomical units. Despite this complex dust structure, no corresponding gas emission was detected, suggesting that if an embedded planet is shaping this region, it must have an exceptionally low mass.

Key findings
- The dust blob at 52 astronomical units moves in harmony with the disk's rotation.
- High-resolution imaging resolves the blob into a double-peaked structure.
- Observations confirm no significant radial movement of the dust over four years.
- The absence of associated gas signals implies any potential planet present has a very low mass.

Scientific study

Resolved Structure and Orbital Motion of a Localized 1 au-scale Dust Accumulation in the Protoplanetary Disk around TW Hya (external link)