Abstract
We examine the hypothesis that the red near-infrared colors of some L dwarfs could be explained by a "dust haze" of small particles in their upper atmospheres. This dust haze would exist in conjunction with the clouds found in dwarfs with more typical colors. We developed a model that uses Mie theory and the Hansen particle size distributions to reproduce the extinction due to the proposed dust haze. We apply our method to 23 young L dwarfs and 23 red field L dwarfs. We constrain the properties of the dust haze including particle size distribution and column density using Markov Chain Monte Carlo methods. We find that sub-micron-range silicate grains reproduce the observed reddening. Current brown dwarf atmosphere models include large-grain (1-100 μm) dust clouds but not sub-micron dust grains. Our results provide a strong proof of concept and motivate a combination of large and small dust grains in brown dwarf atmosphere models.
Original language | English (US) |
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Article number | 96 |
Journal | Astrophysical Journal |
Volume | 830 |
Issue number | 2 |
DOIs | |
State | Published - Oct 20 2016 |
Externally published | Yes |
Keywords
- brown dwarfs
- dust, extinction
ASJC Scopus subject areas
- Astronomy and Astrophysics
- Space and Planetary Science