X-wind Transport Of Chondrules And CAIs Of The Solar System

Details X-wind Transport Of Chondrules And CAIs Of The Solar System X-wind Transport Of Chondrules And CAIs Of The Solar System

Oct 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010dps....42.2402h&link_type=abstract

American Astronomical Society, DPS meeting #42, #24.02; Bulletin of the American Astronomical Society, Vol. 42, p.957

Astronomy and Astrophysics

Astronomy

Scientific paper

It has been suggested that chondrules and calcium-aluminum-rich inclusions (CAIs) were formed at the inner edge of the protoplanetary disk and then entrained in magnetocentrifugal X-winds. We study trajectories of such solid bodies with the consideration of the central star gravity, the protoplanetary disk gravity, and the gas drag of the wind. The efficiency of the gas drag depends on a parameter η, which is the product of the solid body size and density. We find that the gravity of the protoplanetary disk has a non-negligible effect on the trajectories. If a solid body re-enters the flared disk, the re-entering radius depends on the stellar magnetic dipole moment, η, and the disk's gravity. The disk's gravity can make the re-entering radius lower by up to 30%. We find a η threshold for any particular configuration of the X-wind, below which the solid bodies will be expelled from the planetary system. Only the solid bodies with a η larger than but very close to the threshold η can be launched to a re-entering radius larger than 1 AU. This size-sorting effect may explain why chondrules come with a narrow range of sizes within each chondritic class. In addition, our calculations show that CAIs originally smaller than ˜0.2 cm must have been ejected from the Solar system by X-winds. Therefore we propose the disaggregation of CAIs at the accretion to the asteroids to explain the size distributions of CAIs in chondrites.

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