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dc.contributorDepartment of Astronomy, University of Florida, Gainesville, FL, 32611, US
dc.contributorNSF's National Optical-Infrared Astronomy Research Laboratory, Tucson, AZ, 85719, US
dc.contributorArmagh Observatory and Planetarium, College Hill, Armagh, BT61 9DG
dc.contributor.authorDermott, Stanley F.
dc.contributor.authorLi, Dan
dc.contributor.authorChristou, Apostolos A.
dc.date.accessioned2024-11-08T13:35:26Z
dc.date.available2024-11-08T13:35:26Z
dc.date.issued2024-01-01T00:00:00Z
dc.identifier.doi10.1017/S1743921323003940
dc.identifier.other2024IAUS..382...86D
dc.identifier.other10.1017/S1743921323003940
dc.identifier.other0000-0002-0027-6248
dc.identifier.other-
dc.identifier.urihttp://hdl.handle.net/20.500.14302/2143
dc.description.abstractThe asteroid belt is a unique source of information on some of the most important questions facing solar system science. These questions include the sizes, numbers, types and orbital distributions of the planetesimals that formed the planets, and the identification of those asteroids that are the sources of meteorites and near-Earth asteroids. Answering these questions requires an understanding of the dynamical evolution of the asteroid belt, but this evolution is governed by a complex interplay of mechanisms that include catastrophic disruption, orbital evolution driven by Yarkovsky radiation forces, and chaotic orbital evolution driven by gravitational forces. While the timescales of these loss mechanisms have been calculated using estimates of some critical parameters that include the thermal properties, strengths and mean densities of the asteroids, we argue here that the uncertainties in these parameters are so large that deconvolution of the structure of the asteroid belt must be guided primarily by observational constraints. We argue that observations of the inner asteroid belt indicate that the size-frequency distribution is not close to the equilibrium distribution postulated by Dohnanyi (<xref rid=ref10 ref-type=bibr>1969</xref>). We also discuss the correlations observed between the sizes and the orbital elements of the asteroids. While some of these correlations are significant and informative, others are spurious and may arise from the limitations of the Hierarchical Clustering Method that is currently used to define family membership.
dc.publisherIAU Symposium
dc.titleDeconvolving the complex structure of the asteroid belt
dc.typeinproceedings
dc.source.journalIAUS
dc.source.journalIAUS..382
dc.source.volume382
dc.identifier.bibcode2024IAUS..382...86D


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