Physics – Geophysics
Scientific paper
Jun 2011
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011jgre..11606004s&link_type=abstract
Journal of Geophysical Research, Volume 116, Issue E6, CiteID E06004
Physics
Geophysics
Mathematical Geophysics: Numerical Approximations And Analysis (4260), Mineralogy And Petrology: Hydrothermal Systems (0450, 1034, 3017, 4832, 8135, 8424), Planetary Sciences: Fluid Planets: Magnetic Fields And Magnetism, Planetary Sciences: Comets And Small Bodies: Ices, Planetary Sciences: Solar System Objects: Asteroids (4308)
Scientific paper
Carbonaceous chondrites are considered to be the most primitive meteorites that contain some of the earliest formed solar system phases, e.g., Ca-Al-rich inclusions and chondrules. The parent bodies of the carbonaceous chondrites are traditionally known to have experienced aqueous alteration. However, the recent paleomagnetic records of the CV chondrite, Allende, indicate remnant magnetism that suggests that these chondrites possibly evolved on the crustal region of a partially differentiated asteroid having a convective molten iron core. We present results based on our comprehensive numerical simulations of the scenario involving melting and planetary differentiation of asteroids. The possibility of a sizable carbonaceous chondritic crust on these differentiated bodies is explored. The simulations indicate that it could be possible to explain the paleomagnetic records of the chondrites by the dynamo-generated magnetic field from the convective molten iron core. Apart from the slow linear accretion scenario, we envisage a scenario involving two episodes of accretion of the asteroids. An early rapid accretion of the asteroids in the initial stage, perhaps within the initial ˜2 Myr, would produce a sizable molten iron core subsequent to differentiation to produce the required magnetic fields. This would be followed by a slow accretion of consolidated chondritic crust, perhaps over several million years. There is also a possibility of the disrupted expulsion of the chondritic crust by the internal pressures generated by gases released during hydration/dehydration reactions.
Gupta Gopal
Sahijpal Sandeep
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