The origin of chondrules at Jovian resonances

Science

Volumn 279, Issue 5351, 1998, Pages 681-684

  Weidenschilling, S J ^a   Marzari, F ^b   Hood, L L ^c  

^a PLANETARY SCIENCE INSTITUTE   (United States)

^b UNIVERSITY OF PADOVA   (Italy)

^c UNIVERSITY OF ARIZONA   (United States)

Author keywords

[No Author keywords available]

Indexed keywords

ISOTOPE; SILICATE;

CHONDRULE; ISOTOPIC DATING; JUPITER; SOLAR NEBULA;

ARTICLE; ASTRONOMY; COSMOS; PRIORITY JOURNAL; TIME;

EID: 0032579274     PISSN: 00368075     EISSN: None     Source Type: Journal    
DOI: 10.1126/science.279.5351.681     Document Type: Article

References (44)

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21. A radial pressure gradient causes the gaseous component of the nebula to rotate at slightly less than the Keplerian orbital velocity. Solid objects are subjected to gas drag, causing them to lose angular momentum and move inward [I. Adachi, C. Hayashi, K. Nakazawa, Prog. Theor. Phys. 56, 1756 (1976); S. J. Weidenschilling, Mon. Not. R. Astron. Soc. 180, 57 (1977)].
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31. -3 cm) grains are accelerated quickly because of their large area:mass ratio and experience little heating. Bodies larger than approximately centimeter size are heated too slowly to be melted by transient shocks.
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39. Our cases were computed in three dimensions, with initial inclinations between 0° and 1°. There was no significant increase in mean inclination during evolution in resonance.
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44. We thank T. Swindle, T. V. Ruzmaikina, and J. A. Wood for discussions. Supported by NASA (S.J.W. and L.L.H.) and the Italian Space Agency (P.M.). This is Planetary Science Institute Contribution 343.