Journal
ASTROPHYSICAL JOURNAL LETTERS
Volume 706, Issue 1, Pages L46-L51Publisher
IOP PUBLISHING LTD
DOI: 10.1088/0004-637X/706/1/L46
Keywords
binaries: general; circumstellar matter; methods: numerical; stars: formation; stars: general; stars: low-mass, brown dwarfs
Categories
Funding
- McMaster University
- Natural Sciences and Engineering Research Council of Canada
- ASC/Alliances Center for Astrophysical Thermonuclear Flashes at the University of Chicago
- National Science Foundation [PHY05-51164]
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In star formation, magnetic fields act as a cosmic angular momentum extractor that increases mass accretion rates onto protostars and, in the process, creates spectacular outflows. However, recently it has been argued that this magnetic brake is so strong that early protostellar disks-the cradles of planet formation-cannot form. Our three-dimensional numerical simulations of the early stages of collapse (less than or similar to 10(5) yr) of overdense star-forming clouds form early outflows and have magnetically regulated and rotationally dominated disks ( inside 10 AU) with high accretion rates, despite the slip of the field through the mostly neutral gas. We find that in three dimensions magnetic fields suppress gravitationally driven instabilities that would otherwise prevent young, well-ordered disks from forming. Our simulations have surprising consequences for the early formation of disks, their density and temperature structure, the mechanism and structure of early outflows, the flash heating of dust grains through ambipolar diffusion, and the origin of planets and binary stars.
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