Mathematics – Probability
Scientific paper
Oct 2007
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007dps....39.1302t&link_type=abstract
American Astronomical Society, DPS meeting #39, #13.02; Bulletin of the American Astronomical Society, Vol. 39, p.432
Mathematics
Probability
Scientific paper
By virtue of their landing on Earth, meteorites reside in near-Earth object (NEO) orbits prior to their arrival. Thus the population of observable NEOs most likely gives the best representation of meteorite source bodies. By linking meteorites to NEOs, and linking NEOs to their most likely main-belt source regions, we seek to gain insight into the original solar system sources for different meteorite classes. To forge the first link between meteorites and NEOs, we have developed a three dimensional method for quantitative comparisons between laboratory measurements of meteorites and telescopic measurements of near-Earth objects (NEOs). We utilize meteorite spectra from the Reflectance Experiment Laboratory (RELAB) database and NEO data from the SpeX instrument on the NASA IRTF. Using the Modified Gaussian Model (MGM) (Sunshine et al. 1993, JGR 98, 9075) as a mathematical tool (with no mineralogy interpretation), we treat asteroid and meteorite spectra identically in the calculation of 1-micron and 2-micron geometric band centers and their band area ratios (BARs). We fit the continuum as a linear function in wavenumber space. We choose to include the geometric center of the band in this study in order to examine the asymmetry of the bands. Using this numerical data we can examine the differences of the H, L, LL and HED meteorite classes. For each NEO spectrum, we assign a set of probabilities for it being related to each of these classes, yielding probability distributions for our NEO data set being related to H, L, LL, and HED meteorites. Our meteorite correlation distribution is then convolved with an NEO source region model (Bottke et al. 2002, Icarus 156, 399) to shed light on connections between these meteorite classes and their asteroid belt origins.
Binzel Richard P.
Thomas Cristina A.
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