GROWTH OF GRAINS IN BROWN DWARF DISKS

Journal Article · Sun Sep 01 00:00:00 EDT 2013 · Astrophysical Journal Letters

DOI:https://doi.org/10.1088/2041-8205/774/1/L4· OSTI ID:22136556

Meru, Farzana ^[1]; Galvagni, Marina ^[2]; Olczak, Christoph ^[3]

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1. Institut fuer Astronomie, ETH Zuerich, Wolfgang-Pauli-Strasse 27, 8093 Zuerich (Switzerland)
2. Institute of Theoretical Physics, Universitaet Zuerich, Winterthurerstrasse 190, 8057 Zuerich (Switzerland)
3. Astronomisches Rechen-Institut (ARI), Zentrum fuer Astronomie Universitaet Heidelberg, Moenchhofstrasse 12-14, D-69120 Heidelberg (Germany)

We perform coagulation and fragmentation simulations using the new physically motivated model by Garaud et al. 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 millimeter sizes in brown dwarf disks, as seen in T Tauri disks.

• OSTI ID: 22136556
• Journal Information: Astrophysical Journal Letters, Vol. 774, Issue 1; Other Information: Country of input: International Atomic Energy Agency (IAEA); ISSN 2041-8205
• Country of Publication: United States
• Language: English

Related Subjects

79 ASTROPHYSICS
COSMOLOGY AND ASTRONOMY
DWARF STARS
FRAGMENTATION
GRAIN GROWTH
MASS
MATTER
PROTOPLANETS
SIMULATION