The Orbits of Meteorites from Natural Thermoluminescence

• Published in: Icarus (New York, N.Y. 1962) Vol. 125; no. 2; pp. 281 - 287
• Main Authors: Benoit, P.H., Sears, D.W.G.
• Format: Journal Article
• Language: English
• Published: Headquarters Elsevier Inc 01-02-1997
• Subjects: Astrophysics
• ISSN: 0019-1035; 1090-2643
• DOI: 10.1006/icar.1996.5622

The natural thermoluminescence (TL) of meteorites reflects their irradiation and thermal histories. Virtually all ordinary chondrites have been irradiated long enough to have reach saturation natural TL levels, and thus natural TL levels in these meteorites are determined largely by thermal history. The primary heat source for most meteorites is the Sun, and thus natural TL levels are determined primarily by the closest approach to the Sun, i.e., perihelion. By converting natural TL levels to perihelia, using an assumed albedo typical of meteoroid bodies, it is found that most ordinary chondrites had perihelia of 0.85 to 1.0 AU prior to reaching Earth. This range is similar to that calculated from meteor and fireball observations. All common classes of ordinary chondrites exhibit similar perihelia distributions; however, H and LL chondrites that fell in the local morning differ in their natural TL distribution from those that fell in the local afternoon and evening. This is consistent with earlier suggestions that time of fall reflects orbital distribution. The data also suggest that the orbits of some of the H chondrites cluster and may have come from a debris “stream” of meteoroids. If meteorites can exist in “orbital groups,” significant changes in the types and number of meteorites reaching Earth could occur on the <105-year time scale.