Computer Science
Scientific paper
Mar 1996
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996lpi....27..219c&link_type=abstract
Lunar and Planetary Science, volume 27, page 219
Computer Science
3
Grains: Interstellar, Solar Nebula, Solar System: Formation
Scientific paper
Major fractions of the primitive meteorites experienced temperatures high enough to melt or evaporate them. Ubiquitous chemical fractionations are plausibly the result of an early, hot epoch of solar nebular evolution, and chondrules are apparently the products of localized heating in the proto-solar environment. Yet such processed components coexist with interstellargrains, some of which are essentially unscathed by cosmogonic events. Such grains must have avoided or survived at least three potentially destructive environments through which most solar system material passed: the collapsing protosolar cloud, the accretion shock, and the nebula itself. We are examining theoretical models of these environments with the aim of determining what factors affect interstellar grain survival; what patterns one might expect to find in the abundances, type and composition of interstellar material in primitive meteorites; and what can be deduced about the formation of the solar system if such patterns exist. Rigorous calculations of radiative heat transfer in model protosolar envelopes are used to determine the pre-shock survival distances of interstellar components. Shock destruction is evaluated from the detailed shock models of Neufeld and Hollenbach. Nebula midplane temperatures are calculated from simple radiative models, extended to include the backheating effects of the envelope. The primary environmental determinant of survivability is the accretion rate through the nebula, which affects the thermal state of both the nebula and the collapsing cloud. During periods of rapid accretion, silicate grains might survive collapse and the accretion shock to within 2 AU, but would be destroyed in the nebula to distances beyond the terrestrial planet region. During periods of very slow accretion (mass buildup in the disk), those grains could remain intact to well within 1 AU.
Cassen Pat
Chick Kenneth M.
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