Abstract
We present results from the most complex hydrodynamical star formation calculation performed to date. It follows the collapse and fragmentation of a large-scale turbulent molecular cloud to form dozens of stars and brown dwarfs. It resolves all fragmentation down to the opacity limit, binary stars with separations as small as 1 AU, and circumstellar disks with radii down to approximate to 10 AU. In this proceedings, we examine the formation mechanism of the brown dwarfs-and compare the initial mass function and the properties of the brown dwarfs with observations.
Original language | English |
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Pages (from-to) | 27-30 |
Number of pages | 4 |
Journal | BROWN DWARFS |
Publication status | Published - 2003 |
Keywords
- INITIAL MASS FUNCTION