ALMA and CARMA observations of Brown Dwarfs disks: testing the models of dust evolution

TL;DR

This study uses ALMA and CARMA observations to analyze dust properties and disk structures around brown dwarfs, providing critical tests for models of early planet formation in low-mass environments.

Contribution

It presents the first observational results targeting brown dwarf disks to test dust evolution models in planet formation.

Findings

Initial observational data on brown dwarf disks.

Insights into dust coagulation and fragmentation processes.

Constraints on models of planetesimal formation in low-mass disks.

Abstract

The first steps toward planet formation involve the coagulation of small microscopic grains into larger and larger pebbles and rocks in gas-rich disks around young stars and brown dwarfs. Observations in the sub-millimeter can trace mm/cm-sized pebbles in the outer disks, and investigate the mechanisms of coagulation/fragmentation and radial migration of these solids. These represent key, yet not fully understood ingredients for our understanding of the formation of planetesimals, the building blocks of planets. Here we present the first results from an observational program using the ALMA and CARMA sub-mm/mm interferometers aimed at characterizing the dust properties and disk structure of young disks around brown dwarfs and very low mass stars. Given the physical conditions expected for these disks, they represent critical test beds for the models of the early stages of planet formation in proto-planetary disks.