Other
Scientific paper
Dec 2004
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004dps....36.1710b&link_type=abstract
American Astronomical Society, DPS meeting #36, #17.10; Bulletin of the American Astronomical Society, Vol. 36, p.1103
Other
1
Scientific paper
Recent spectral observations of some Kuiper Belt Objects (KBOs) (Boehnhardt et al.: 2002, Proc. of ACM 2002, 47-50; Fornasier S. et al., 2004, Astron. Astrophys. 421, 353-363) discovered characteristic absorption bands at 4300 and 6000-8000Å in reflectance spectra of the bodies. Spectral positions and other parameters of the features are similar to those found in reflectance spectra of terrestrial phyllosilicates (e. g., Clark et al., 1990, J. Geophys. Res. 95, 12653-12680; Busarev et al., 2004, The new ROSETTA targets (L. Colangeli et al., eds.), 79-83), CI- and CM-carbonaceous chondrites (e. g., Busarev and Taran, 2002, Proc. of ACM 2002, 933-936), primitive C-, P-, D-, F- and G-class asteroids (Vilas and Gaffey, 1989, Science 246, 790-792) and hydrated M-, S- and E-class asteroids (Busarev and Taran, 2002, Proc. of ACM 2002, 933-936). Hence, these absorption bands may be considered as universal indicators of hydrated silicates on celestial solid bodies including KBOs. However, before phyllosilicates were formed, an aqueous media should spring up and exist a considerable time in the bodies. One more important factor for the spectral features of hydrated silicates to be observed, it is probably an aqueous separation of silicate and darkening CHON (PAH plus more light organic compounds) components in the bodies. To check the assumptions we have performed some calculations (Busarev et al., 2003, Earth, Moon, and Planets 92, 345-357) applicable to KBOs and analogous silicate-icy bodies existed for the first time in the formation zones of neighbouring giant planets. According to the calculations, the decay of the short-lived 26Al at the early stage of the bodies' evolution and their mutual collisions (at velocities >1.5 km s-1) at the subsequent stage were probably the main sources of heating sufficient for melting water ice in their interiors. Because of these processes, an internal ocean of liquid water covered with ˜10-km crust of dirty ice could originate in large KBOs (R>100 km) for about 106 yr and exist a few Myr till their freezing. The water ocean would be vigorously convective (Ra ˜1021) and the temperature should stabilize near 277-280K owing to the rapid radial heat transport through the ocean. A thin nonconvective layer could exist only at the top of the ocean because of the negative thermal expansion coefficient of water between 273 and 277K. As a result, dissolution and/or floating of the main part of a CHON component and sedimentation of silicate particles could occur. It probably finished in large KBOs by formation of a silicate core ( ˜0.7 radius of a body) covered with a water-ice shell enriched with organics. Crushing and removing icy covers under collisions and exposing KBOs' interiors with increased silicate content could facilitate detection of phyllosilicate spectral features.
Busarev Vladimir V.
Dorofeeva V. A.
Makalkin A. B.
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