2006/03/24 by Alexander Scholz, A. Scholz, Ray Jayawardhana +1 · 4 citations
Physics and Astronomy · #Astro and Planetary Science #Astronomy #Astrophysics #Astrophysics and Star Formation Studies #Brown dwarf #Millimeter #Physics #Stars #Stellar, planetary, and galactic studies #astro-ph
paper · pdf · doi:10.1086/504464
published as Astrophys.J. 645 (2006) 1498-1508 · 29 pages, 4 figures, accepted for publication in ApJ, typo in caption for Fig. 4 corrected
arxiv created 2006/03/24 · openalex publication_date 2006/07/07 · arxiv updated 2009/12/01 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/06
We have carried out sensitive 1.3 mm observations of 20 young brown dwarfs in the Taurus star-forming region, representing the largest sample of young substellar objects targeted in a deep millimeter-continuum survey to date. Under standard assumptions, the masses of brown dwarf disks range from ≲0.4 to several Jupiter masses. Their relative disk masses are comparable to those derived for coeval low-mass stars; most of them are in the ≲1%-5% range, and there is no clear change of relative disk mass with object mass from 0.015 to 3 M ☉ . Specifically, we do not find evidence for disk truncation, as would be expected in the ejection scenario for brown dwarf origin, although the signature of ejection may be hidden in our nondetections. We use the millimeter fluxes, complemented by mid-infrared data from the Spitzer Space Telescope to construct spectral energy distributions (SEDs) for six of our sources, and model those SEDs with a Monte Carlo radiative transfer code. We find that the SEDs in the mid-infrared often exhibit lower flux levels than predicted by hydrostatic models, implying dust settling to the disk midplane. What is more, at least 25% of our targets are likely to have disks with radii >10 AU; models with smaller disks cannot reproduce the millimeter fluxes. This result is in contrast to the results of some simulations of the ejection scenario for brown dwarf formation that suggest only ~5% of ejected objects would harbor disks larger than 10 AU. Our findings imply that ejection is probably not the dominant formation process, but may still be relevant for some brown dwarfs.