English (United Kingdom)

https://curated-unify.zendy.io/wp-json/zendy-region/v1/featured_content/oa?rat=en

https://curated-unify.zendy.io/wp-json/zendy-region/v1/highlighted_journal/

Global: Zendy Plus annual

Presents the access of premium content as premium feature

Premium Content

Presents the keyphrase highlighting as premium feature

Keyphrase Highlighting

Presents the summarisation as premium feature

Summarisation

Insights

Presents the pdf analysis as premium feature

PDF Analysis

Presents the zaia usage as premium feature

ZAIA

Global: Zendy Plus monthly

Global: Zendy Tools annual

Global: Zendy Tools monthly

Global: Zendy Free Plan

Characterizing the physical properties of dust grains in a protoplanetarydisk is critical to comprehending the planet formation process. Our studypresents ALMA high-resolution observations of the young protoplanetary diskaround DG Tau at a 1.3 mm dust continuum. The observations, with a spatialresolution of $\approx 0.04''$, or $\approx5$ au, revealed a geometrically thinand smooth disk without substantial substructures, suggesting that the diskretains the initial conditions of the planet formation. To further analyze thedistributions of dust surface density, temperature, and grain size, weconducted a multi-band analysis with several dust models, incorporating ALMAarchival data of the 0.87 mm and 3.1 mm dust polarization. The results showedthat the Toomre $Q$ parameter is $\lesssim2$ at a 20 au radius, assuming adust-to-gas mass ratio of 0.01. This implies that a higher dust-to-gas massratio is necessary to stabilize the disk. The grain sizes depend on the dustmodels, and for the DSHARP compact dust, they were found to be smaller than$\sim400$ $\mu$m in the inner region ($r\lesssim20$ au), while exceeding largerthan 3 mm in the outer part. Radiative transfer calculations show that the dustscale height is lower than at least one-third of the gas scale height. Thesedistributions of dust enrichment, grain sizes, and weak turbulence strength mayhave significant implications for the formation of planetesimals throughmechanisms such as streaming instability. We also discuss the CO snowlineeffect and collisional fragmentation in dust coagulation for the origin of thedust size distribution.

Dust enrichment and grain growth in a smooth disk around the DG Tau protostar revealed by ALMA triple bands frequency observations