Big Chemical Encyclopedia

Chemical substances, components, reactions, process design ...

Articles Figures Tables About

Chondrules temperatures

The O isotopes show signihcant heterogeneity between the different meteorite classes (Fig. 8a Clayton et al. 1976, 1977). Differences are small, but, each chondrite group has a distinct bulk O isotopic composition. O isotopes also indicate the close ties between the Earth and the Moon. O therefore can be used to identify members of a family that formed from a common reservoir, which is the definition of a tracer. Such differences are also formd between chondrules within the same meteorites related to their size (Gooding et al. 1983). This is a survival of the initial isotopic heterogeneity in already high temperature processed materials like chondrules. [Pg.45]

Figure 16. Plot of TL sensitivity against peak temperature and peak width for chondrules separated from the Dhajala meteorite (type 3.8). Because the chondrule masses vary over several orders of magnitude, their TL data have been divided by mass. (Reprinted with permission from Ref. 26. Copyright 1984 Pergamon Press.)... Figure 16. Plot of TL sensitivity against peak temperature and peak width for chondrules separated from the Dhajala meteorite (type 3.8). Because the chondrule masses vary over several orders of magnitude, their TL data have been divided by mass. (Reprinted with permission from Ref. 26. Copyright 1984 Pergamon Press.)...
Figure 5.5 Winds in the solar nebula might be one of the possible processes responsible for the mixing of hot and cold components found in both meteorites and comets. Meteorites contain calcium-aluminum-rich inclusions (CAIs, formed at about 2000 K) and chondrules (formed at about 1650K), which may have been created near the proto-Sun and then blown (gray arrows) several astronomical units away, into the region of the asteroids between Mars and Jupiter, where they were embedded in a matrix of temperature-sensitive, carbon-based cold components. The hot component in comets, tiny grains of annealed silicate dust (olivine) is vaporized at about 1600 K, suggesting that it never reached the innermost region of the disk before it was transported (white arrows) out beyond the orbit of Pluto, where it was mixed with ices and some unheated silicate dust ( cold components). Vigorous convection in the accretion disk may have contributed to the transport of many materials and has been dramatically confirmed by the Stardust mission (Nuth 2001). Figure 5.5 Winds in the solar nebula might be one of the possible processes responsible for the mixing of hot and cold components found in both meteorites and comets. Meteorites contain calcium-aluminum-rich inclusions (CAIs, formed at about 2000 K) and chondrules (formed at about 1650K), which may have been created near the proto-Sun and then blown (gray arrows) several astronomical units away, into the region of the asteroids between Mars and Jupiter, where they were embedded in a matrix of temperature-sensitive, carbon-based cold components. The hot component in comets, tiny grains of annealed silicate dust (olivine) is vaporized at about 1600 K, suggesting that it never reached the innermost region of the disk before it was transported (white arrows) out beyond the orbit of Pluto, where it was mixed with ices and some unheated silicate dust ( cold components). Vigorous convection in the accretion disk may have contributed to the transport of many materials and has been dramatically confirmed by the Stardust mission (Nuth 2001).

See other pages where Chondrules temperatures is mentioned: [Pg.99]    [Pg.99]    [Pg.100]    [Pg.22]    [Pg.162]    [Pg.164]    [Pg.164]    [Pg.176]    [Pg.176]    [Pg.94]    [Pg.186]    [Pg.353]    [Pg.158]    [Pg.208]    [Pg.214]    [Pg.236]    [Pg.317]    [Pg.324]    [Pg.489]    [Pg.490]    [Pg.492]    [Pg.494]    [Pg.494]    [Pg.513]    [Pg.88]    [Pg.160]    [Pg.165]    [Pg.216]    [Pg.219]    [Pg.87]    [Pg.88]    [Pg.149]    [Pg.208]    [Pg.218]    [Pg.218]    [Pg.219]    [Pg.220]    [Pg.220]    [Pg.224]    [Pg.225]    [Pg.230]    [Pg.231]    [Pg.233]    [Pg.243]    [Pg.246]    [Pg.247]    [Pg.247]    [Pg.247]   
See also in sourсe #XX -- [ Pg.208 ]




SEARCH



Chondrules

© 2024 chempedia.info