Evolution of young brown dwarf disks in the mid-infrared

M. F. Sterzik, I. Pascucci, D. Apai, N. Van Der Bliek, C. P. Dullemond

Research output: Contribution to journalArticlepeer-review

62 Scopus citations


We have imaged two bona-fide brown dwarfs with TReCS/GEMINI-S and find mid-infrared excess emission that can be explained by optically thick dust disk models. In the case of the young (≈2 Myr) Cha Hal we measure fluxes at 10.4 μm and 12.3 μm that are fully consistent with a standard flared disk model and prominent silicate emission. For the μ10 Myr old brown dwarf 2MASS1207-3932 located in the TW Hydrae association we find excess emission at 8.7 μm and 10.4 μm with respect to the photosphere, and confirm disk accretion as a likely cause of its strong activity. Disks around brown dwarfs likely last at least as long as their low-mass stellar counterparts in the T-Tauri phase. Grain growth, dust settling, and evolution of the geometry of brown dwarf disks may appear on a timescale of 10 Myr and can be witnessed by observations in the mid-infrared.

Original languageEnglish (US)
Pages (from-to)245-250
Number of pages6
JournalAstronomy and astrophysics
Issue number1
StatePublished - Nov 2004


  • Accretion, accretion disks
  • Stars: formation
  • Stars: low-mass, brown dwarfs

ASJC Scopus subject areas

  • Astronomy and Astrophysics
  • Space and Planetary Science


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