# Effects of Ringed Structures and Dust Size Growth on Millimeter Observations of Protoplanetary Disks

## TL;DR

This study uses hydrodynamical simulations to show that ringed structures and dust growth significantly influence millimeter observations of protoplanetary disks, explaining low spectral indices and brightness variations.

## Contribution

It demonstrates how ringed structures and dust size evolution jointly affect millimeter flux and spectral indices, providing insights into disk observations and planet formation processes.

## Key findings

- Ringed structures slow dust radial drift and promote growth.
- High fragmentation velocity disks can have mm spectral index ~2.0.
- Multiple rings can produce disks with spectral indices below 2.5.

## Abstract

The growth of solids from sub-micron to millimeter and centimeter sizes is the early step toward the formation of planets inside protoplanetary disks (PPDs). However, such processes and their potential impact on the later stages of solid growth are still poorly understood. In this work, we test the hypothesis that most disks contain at least one ringed structure with a relative small radius. We have carried out a large family of 1D two-fluid (gas+dust) hydrodynamical simulations by evolving the gas and dust motion self-consistently while allowing dust size to evolve via coagulation and fragmentation. We investigate the joint effects of ringed structures and dust size growth on the overall sub-millimeter and millimeter (mm) flux and spectral index of PPDs. Ringed structures slow down the dust radial drift and speed up the dust growth. In particular, we find that those unresolved disks with a high fragmentation velocity ($\sim10\ {\rm m~s^{-1}}$) and a high dust surface density ($\sim10\ {\rm g\ cm^{-2}}$ in the ring) can have mm spectral indices as low as $\sim2.0$, consistent with mm observations of faint disks in nearby star forming regions. Furthermore, disks with more than one ringed structure can potentially reproduce brighter disks with spectral indices lower than $\sim2.5$. Future multi-wavelength high-resolution observations of these low spectral index sources can be used to test the existence of the ringed structures in the unresolved disks and differentiate the effects of dust size growth from optical depth.