Asteroid Family Physical Properties

Abstract

An asteroid family is typically formed when a larger parent body undergoes a catastrophic collisional disruption, and as such family members are expected to show physical properties that closely trace the composition and mineralogical evolution of the parent. Recently a number of new datasets have been released that probe the physical properties of a large number of asteroids, many of which are members of identified families. We review these data sets and the composite properties of asteroid families derived from this plethora of new data. We also discuss the limitations of the current data, and the open questions in the field.

Chapter to appear in the Space Science Series Book: Asteroids IV

References in corpus (10)

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Cited by in corpus (13)

• Asteroid Taxonomy from Cluster Analysis of Spectrometry and Albedo
• Olivine-dominated A-type asteroids in the Main Belt: Distribution, Abundance and Relation to Families
• Impact bombardment chronology of the terrestrial planets from 4.5 Ga to 3.5 Ga
• Asteroid Families: properties, recent advances and future opportunities
• Yarkovsky V-shape identification of asteroid families
• Asteroid thermal modeling in the presence of reflected sunlight with an application to WISE/NEOWISE observational data
• Modification of the composition and density of Mercury from late accretion
• High-Resolution Observations of Bright Boulders on Asteroid Ryugu: 1. Size Frequency Distribution and Morphology
• A new estimate for the age of highly-siderophile element retention in the lunar mantle from late accretion
• Photometric Confirmation and Characterization of the Ennomos Collisional Family in the Jupiter Trojans
• Analysing the Main Belt asteroid distributions by wavelets
• A pre-flyby view on the origin of asteroid Donaldjohanson, a target of the NASA Lucy mission
• Size-Based Spectrophotometric Analysis of the Polana-Eulalia Complex