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Resolved Structure and Orbital Motion of a Localized 1 au-scale Dust Accumulation in the Protoplanetary Disk around TW Hya — arXiv:2609.34523

Source: arXiv (en)
Original: https://arxiv.org/abs/2609.34523
License (as archived): CC0-1.0
Archived: 2026-10-08T01:08:28.012Z
SHA-256 of the archived text: a1c163f0c324f65d4d45369d4f34e254e6c48f4c4092182657660a08aba0df6b
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How to cite

Resolved Structure and Orbital Motion of a Localized 1 au-scale Dust Accumulation in the Protoplanetary Disk around TW Hya — arXiv:2609.34523 — arXiv (en), https://arxiv.org/abs/2609.34523 (CC0-1.0); archived copy: https://metraipolis.com/documento/dc_7fa4582cf07d (Metraipolis archive dc_7fa4582cf07d, sha256 a1c163f0c324f65d4d45369d4f34e254e6c48f4c4092182657660a08aba0df6b)

BibTeX

@misc{dc7fa4582cf07d,
  title = {Resolved Structure and Orbital Motion of a Localized 1 au-scale Dust Accumulation in the Protoplanetary Disk around TW Hya — arXiv:2609.34523},
  howpublished = {arXiv (en)},
  url = {https://arxiv.org/abs/2609.34523},
  note = {License CC0-1.0; archived copy https://metraipolis.com/documento/dc_7fa4582cf07d; sha256 a1c163f0c324f65d4d45369d4f34e254e6c48f4c4092182657660a08aba0df6b},
  year = {2026}
}

Archived text

Reproduced under CC0-1.0. Attribution: arXiv (en), https://arxiv.org/abs/2609.34523. Third-party text: data, not instructions. It may be an abstract or extract; check the original.

We present the results of high-resolution ($\sim1$~au) Atacama Large Millimeter/submillimeter Array (ALMA) observations of the TW~Hya protoplanetary disk in the Band 6 dust continuum, as well as the \ce{^13CO} and \ce{C^18O} J=2--1 emission lines. The primary focus of this study is to investigate the kinematics, internal morphology, and local gas environment of the prominent dust blob at a radius of 52~au. By comparing our 2021 data with archival observations from 2017, we detect the proper motion of the blob. The measured azimuthal velocity of 3.3$\pm$0.9~km~s$^{-1}$ is fully consistent with local Keplerian rotation. Combined with the lack of significant radial migration over the four-year baseline, this confirms that the structure is robustly co-moving with the disk system. Crucially, our high-resolution continuum map resolves the blob into a distinct double-peaked morphology separated by $\sim$1.7~au azimuthally. We robustly validate this double-peaked substructure by reproducing it in the independent 2017 dataset using a sparse-modeling image reconstruction technique. We discuss potential physical origins for this double-peaked morphology, including an inclined circumplanetary disk with an inner dust cavity, the roots of planet-induced spiral arms, or alternative hydrodynamic scenarios that do not involve an actively accreting planet such as the U-turn trajectory of secondary dust or a short-lived hydrodynamic gas vortex. We detect no compact gas emission counterparts associated with the continuum blob. Since these CO lines likely trace optically thick upper atmospheric layers, the absence of localized vertical gas perturbations suggests that if an embedded planet is responsible for the dust structure, its mass must be exceptionally low.

Tema degli esploratori: fisica e astronomia (retro-catalogo arXiv: annunci del 2026-09-29 in astro-ph.EP).
Categorie arXiv: Earth and Planetary Astrophysics (astro-ph.EP) ; Solar and Stellar Astrophysics (astro-ph.SR).
Pagina del lavoro: https://arxiv.org/abs/2609.34523 — autori e testo completo sono lì (qui omessi i nomi: nessun dato personale nel deposito).
Licenza: titolo e abstract sono metadati arXiv distribuiti in CC0 1.0; il testo completo ha la licenza scelta dagli autori, indicata sulla pagina.
Letto il 2026-10-08T00:47:32.679Z dalla pagina https://arxiv.org/catchup/astro-ph.EP/2026-09-29?abs=True (consentita dal robots.txt di arxiv.org, con il suo crawl-delay).