Recent Origin of the Solar System Dust Bands

By D. Nesvorný, William Bottke, Harold Levison, L. Dones. 2003

175 citations recorded by the source corpus.

View Paper: https://www.semanticscholar.org/paper/7bb543a73044fcef4e52ab6b95c378ca617c93f7

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

In Astronomy and Astrophysics

Citations in the corpus

Resonant Trapping of Planetesimals by Planet Migration: Debris Disk Clumps and Vega’s Similarity to the Solar System (2003, background): “Such events may have been witnessed in the structure of the zodiacal cloud (Dermott et al. 2002; Nesvorný et al. 2003).”
Decay of Planetary Debris Disks (2005, background): “Dermott et al. (2002) and Nesvorný et al. (2003) show that the i ¼ 10 band is probably a result of the breakup of the Veritas asteroid family precursor about 8.3 Myr ago, an object thought to be 140 km in diameter.”
Transience of Hot Dust around Sun-like Stars (2006, background): “This is believed to have been significantly enhanced for timescales of a few Myr following collisions between objects ∼ 100 km in size in the asteroid belt (Nesvorný et al. 2003; Far- ley et al. 2006).”
PRELIMINARY RESULTS FROM NEOWISE: AN ENHANCEMENT TO THE WIDE-FIELD INFRARED SURVEY EXPLORER FOR SOLAR SYSTEM SCIENCE (2011, background): “Some of these bands have been associated with the breakups of asteroids in the Main Belt that lead to the formation of young asteroid families (Nesvorny et al. 2003, 2006b).”
Size-frequency distributions of fragments from SPH/N-body simulations of asteroid impacts: Comparison with observed asteroid families (2007, methodology): “Our formal procedure for determining families is described in Nesvorný et al. (2003).”
Linking the collisional history of the main asteroid belt to its dynamical excitation and depletion (2005, background): “It is responsible for one of the prominent dust bands observed by IRAS (Nesvorný et al., 2002, 2003).”
COLLISIONS BETWEEN GRAVITY-DOMINATED BODIES. I. OUTCOME REGIMES AND SCALING LAWS (2011, background): “Asteroid families and their associated dust bands are believed to have formed in recent catastrophic impact events (Nesvorný et al. 2003).”
Yarkovsky/YORP chronology of asteroid families (2006, methodology): “This representation was used by Vokrouhlický et al. (2002) and Nesvorný et al. (2003, 2005) to estimate the ages of several families (e.g., Eos).”
COMETARY ORIGIN OF THE ZODIACAL CLOUD AND CARBONACEOUS MICROMETEORITES. IMPLICATIONS FOR HOT DEBRIS DISKS (2009, background): “It has been established that the dust bands originate from the youngest asteroid families (Nesvorný et al. 2003, 2008).”
Asteroid family ages (2015, methodology): “In order of estimated age: 1547 (Nele): for this family Brož et al. (2013) give an age < 40 My; Nesvorný et al. (2003) give a constraint ≤ 5 My on the age of the Iannini cluster, which he identified as composed of 18 members not including (1547).”
Steady State Evolution of Debris Disks around A Stars (2007, background): “…of these planetesimal belts since this event is thought to have been relatively slow, with mass falling off due to collisional processing, but with large spikes in the dust content of the inner solar system occurring when two large asteroids collided (Nesvorný et al. 2003; Farley et al. 2006).”
Evidence for asteroid space weathering from the Sloan Digital Sky Survey (2005, methodology): “Nesvorný et al. (2002a, 2003)used this method to determine the ages of the Karin (5.8 ± 0.2 My) and Veritas (8.3± 0.5 My) families, and also found that th tight family associated with (4652) Iannini is probab 5 My old.”
The fossilized size distribution of the main asteroid belt (2003, methodology): “Note that this method has bee successfully used to identify the 5.8 Myr old Karin clu ter and many other main belt families(Nesvorný et al., 2002c, 2003, 2005; Nesvorný and Bottke, 2004).”
Identification and Dynamical Properties of Asteroid Families (2015, unknown): “These considerations allow us to define the V-shape criterion (e.g., Nesvorný et al., 2003).”
The formation of asteroid satellites in large impacts: Results from numerical simulations (2004, background): “…was large enough to uncover the Karin cluster, a cluster of asteroids produced by the breakup of a ∼ 25-km diameter asteroid 5.8 Myr ago (Nesvorný et al., 2002), and several additional asteroid clusters that are also believed to be byproducts of recent disruption events (Nesvorný et al., 2003).”
THE YARKOVSKY AND YORP EFFECTS: Implications for Asteroid Dynamics (2006, methodology): “…hydrocode results of asteroid collisions (Michel et al. 2001), as well as recent asteroid disruption events (e.g., <10 My for Karin and Veritas; Nesvorný et al. 2002a, 2003), are much lower ( 100 m s−1) than those inferred from the orbital positions of more evolved asteroid family members.”