Growth of grains in Brown Dwarf disks

Abstract

We perform coagulation and fragmentation simulations using the new physically-motivated model by Garaud et al. (2013) to determine growth locally in brown dwarf disks. We show that large grains can grow and that if brown dwarf disks are scaled down versions of T Tauri disks (in terms of stellar mass, disk mass and disk radius) growth at an equivalent location with respect to the disk truncation radius can occur to the same size in both disks. We show that similar growth occurs because the collisional timescales in the two disks are comparable. Our model may therefore potentially explain the recent observations of grain growth to millimetre sizes in brown dwarf disks, as seen in T Tauri disks.

6 pages, 4 figures, accepted by ApJL

References in corpus (8)

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• ALMA Observations of the Young Substellar Binary System 2M1207
• Disk Masses and Dust Evolution of Protoplanetary Disks Around Brown Dwarfs
• Breakthrough revisited: investigating the requirements for growth of dust beyond the bouncing barrier
• Modeling the Protoplanetary Disks of Two Brown Dwarfs in the Taurus Molecular Cloud
• VLA observations of the disk around the young brown dwarf 2MASS J044427+2512
• The disk around the brown dwarf KPNO Tau 3
• MINDS. Cha Hα 1, a brown dwarf with a hydrocarbon-rich disk