![]() They come from asteroids and from the surface of the Moon and Mars. Meteorites have their origins in the larger bodies of the solar system. A few rare meteorites come from the Moon and Mars. When asteroids collide, they scatter rock fragments throughout space. Larger pieces of the sky generally come from asteroids, or minor planets. The smallest particles generate very little friction with our atmosphere and drift gently down to the surface. When Earth’s orbit takes us through those dust trails, the material enters our atmosphere and vaporizes. As they orbit the Sun, Comets scatter dust along their paths. The smallest and most plentiful particles come from comets, which contain ice and dust. Anything that survives the trip and lands on the surface is then called a meteorite. The resulting flashes of light in the sky are meteors. The smaller ones burn up because of friction with air molecules. As Earth’s orbit takes us through this debris, pieces of it enter our atmosphere. It is filled with dust shed from comets and fragments of broken asteroids. The space between the planets is not empty. Any reuse of this item in excess of fair use or other copyright exemptions requires express permission of the copyright holder.Pieces of comets and asteroids fall from space and cause the flashes of light in the sky that we see as meteors. Users of this work assume the responsibility for determining copyright status prior to reusing, publishing, or reproducing this item for purposes other than what is allowed by fair use or other copyright exemptions. §107) for non-profit research and educational purposes. This item is protected by copyright but is made available here under a claim of fair use (17 U.S.C. The accuracy and precision of the results compare well with the data reported for the reference Allende bulk samples prepared by the Smithsonian Institution. The samples show less chemical variation than the slabs. The data were evaluated statistically by several methods and the analysis indicates that the Allende meteorite is a well-indurated polymict breccia. The method requires a minimum of half the transmission readings of previous methods and allows many more samples to be exposed on a single spectrographic plate. A method for making background correction on a single spectrum when measuring the spectrographic plates on a densitometer was developed. The method has reduced matrix effects and uses less sample than previous optical emission spectrographic methods. An optical emission spectrographic analysis method using a demountable hollow cathode source was developed. The 108 splits were numbered randomly and analyzed in random order. The homogenized slab material was then split into four splits for each slab. The slabs were crushed and screened through a 60 sieve. Three slabs oriented to obtain the most representative portions were wire sawed from each sample. Nine elements from four geochemical divisions were used in the analyses. Nine samples of six pieces of the meteorite were analyzed spectrochemically for large scale chemical variations. The Allende, Mexico C3(V) is the largest stony meteorite fall recorded.
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