Yarkovsky V-shape identification of asteroid families

Abstract

There are only a few known main belt (MB) asteroid families with ages greater than 2 Gyr (Brož et al. 2013, Spoto et al. 2015). Estimates based on the family producing collision rate suggest that the lack of >2 Gyr-old families may be due to a selection bias in current techniques used to identify families. Family fragments disperse in their orbital elements, semi-major axis, $a$, eccentricity, $e$, and inclination, $i$, due to secular resonances, close encounters with massive asteroids and the non-gravitational Yarkovsky force. This causes the family fragments to be indistinguishable from the background of the main belt making them more difficult to identify with the hierarchical clustering method (HCM) with increasing family age. The discovery of the Eulalia and new Polana families in the inner belt relied on new techniques because Yarkovsky spreading made them too disperse to be identified using the classical HCM. The technique used to discover the new Polana and Eulalia families is modified to identify asteroid families by searching for correlations between $a$ and asteroid diameter, $D$, or absolute magnitude, $H$. A group of asteroids is identified as a collisional family if its boundary in the $a$ vs. 1/$D$ or $a$ vs. $H$ planes has a characteristic V-shape which is due to the size dependent Yarkovsky spreading. The V-shape boundary is identified with two separate techniques. The first identifies a border by measuring the drop between the number of objects inside and outside of the border. The second identifies the V-shape border by measuring the number density of objects in $a$ vs. 1/$D$,$H$ space. The V-shape techniques are demonstrated on known families Erigone, Vesta, Koronis, and families difficult to identify by HCM such as Flora, Baptistina, new Polana, Eulalia and Karin. Application of the technique in a search for >2 Gyr-old families throughout the MB is discussed.

arXiv comment74 pages, 17 figures, accepted for publication in Icarus

References in corpus (44)

• The Wide-field Infrared Survey Explorer (WISE): Mission Description and Initial On-orbit Performance
• A low mass for Mars from Jupiter's early gas-driven migration
• Solar System Objects Observed in the SDSS Commissioning Data
• Main Belt Asteroids with WISE/NEOWISE I: Preliminary Albedos and Diameters
• Collisions Between Gravity-Dominated Bodies: 1. Outcome Regimes and Scaling Laws
• Collisions between Gravity-Dominated Bodies: 2. The Diversity of Impact Outcomes during the End Stage of Planet Formation
• Thermal inertia of near-Earth asteroids and implications for the magnitude of the Yarkovsky effect
• Orbit and Bulk Density of the OSIRIS-REx Target Asteroid (101955) Bennu
• Asteroid families classification: exploiting very large data sets
• Evidence from the asteroid belt for a violent past evolution of Jupiter's orbit
• Formation of asteroid pairs by rotational fission
• The Size Distributions of Asteroid Families in the SDSS Moving Object Catalog 4
• The Yarkovsky and YORP Effects
• Identification and Dynamical Properties of Asteroid Families
• Asteroid family ages
• Dynamical erosion of the asteroid belt and implications for large impacts in the inner solar system
• The Pan-STARRS Moving Object Processing System
• Introducing the Eulalia and new Polana asteroid families: re-assessing primitive asteroid families in the inner Main Belt
• Extreme Sensitivity of the YORP Effect to Small-Scale Topography
• Asteroid thermophysical modeling
• Asteroid family identification using the Hierarchical Clustering Method and WISE/NEOWISE physical properties
• Constraining the cometary flux through the asteroid belt during the late heavy bombardment
• Absolute magnitudes and slope parameters for 250,000 asteroids observed by Pan-STARRS PS1 - preliminary results
• The Influence of Rough Surface Thermal-Infrared Beaming on the Yarkovsky and YORP Effects
• Main Belt Binary Asteroidal Systems With Eccentric Mutual Orbits
• The Dynamical Evolution of the Asteroid Belt
• Coupled Spin and Shape Evolution of Small Rubble-Pile Asteroids: Self-Limitation of the YORP Effect
• On the Ages of Resonant, Eroded and Fossil Asteroid Families
• Constraining the Cratering Chronology of Vesta
• Did the Hilda collisional family form during the late heavy bombardment?
• Revising the age for the Baptistina asteroid family using WISE/NEOWISE data
• An anisotropic distribution of spin vectors in asteroid families
• Collisional family structure within the Nysa-Polana complex
• The Eos family halo
• Collisional Formation and Modeling of Asteroid Families
• Asteroid Family Physical Properties
• Dynamical evolution of the Cybele asteroids
• Defining the Flora Family: Orbital Properties, Reflectance Properties and Age
• The Euphrosyne family's contribution to the low albedo near-Earth asteroids
• Footprints of a possible Ceres asteroid paleo-family
• On the oldest asteroid families in the main belt
• The daily processing of asteroid observations by Gaia
• Chaotic diffusion of the Vesta family induced by close encounters with massive asteroids
• On the Erigone family and the $z_2$ secular resonance

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• An ancient and a primordial collisional family as the main sources of X-type asteroids of the inner Main Belt
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• An automatic approach to exclude interlopers from asteroid families
• A dark asteroid family in the Phocaea region
• Exogenous origin of hydration on asteroid (16) Psyche: The role of hydrated asteroid families
• The discovery and characterization of a kilometre sized asteroid inside the orbit of Venus
• Stability of Jovian Trojans and their collisional families
• Orbit decay of 2-100 au planetary remnants around white dwarfs with no gravitational assistance from planets
• Size-dependent modification of asteroid family Yarkovsky V-shapes
• Initial velocity V-shapes of young asteroid families
• Gaia search for early-formed andesitic asteroidal crusts
• Identification of a 4.3 billion year old asteroid family and planetesimal population in the Inner Main Belt
• Gaia view of primitive inner-belt asteroid families: Searching for the origins of asteroids Bennu and Ryugu
• Evolution of an asteroid family under YORP, Yarkovsky and collisions
• Efficiency characterization of the V-shape asteroid family detection method
• Asteroid spin-states of a 4 Gyr collisional family
• Astrocladistics of the Jovian Trojan Swarms
• Spin states of X-complex asteroids in the inner main belt -- I. Investigating the Athor and Zita collisional families
• A pre-flyby view on the origin of asteroid Donaldjohanson, a target of the NASA Lucy mission
• An ancient L- type family associated to (460) Scania in the Middle Main Belt as revealed by Gaia DR3 spectra