The peculiar case of the Agnia asteroid family

Vokrouhlický, David; Brož, M.; Bottke, W. F.; Nesvorný, David; Morbidelli, Alessandro

doi:10.1016/j.icarus.2006.03.002

Cited by 49 publications

(68 citation statements)

References 47 publications

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“…Nesvorný et al (2015) estimate the age of the Hoffmeister family to be 210 ± 10 Myr, while Spoto et al (2015), using a V-shape criteria, evaluate the family to be 330 ± 100 Myr old, and found no asymmetry between the left and right side of the family semi-major axis distribution, concerning the estimation of the group age. As discussed in Carruba (2016) Monte Carlo methods (Vokrouhlický et al 2006a;Vokrouhlický et al 2006;Vokrouhlický et al 2006c) that simulates the evolution of the family caused by the Yarkovsky and YORP effects, where YORP stands for Yarkovsky-O'Keefe-Radzievskii-Paddack effect, could also be used to obtain estimates of the age and terminal ejection velocities of the family members (these models will be referred as "Yarko-Yorp" models hereafter). However, the age estimates from these methods depend on key parameters describing the strength of the Yarkovsky force, such as the thermal conductivity K and bulk and surface density ρ bulk and ρ surf , that are in many cases poorly known.…”

Section: Physical Propertiesmentioning

confidence: 99%

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The Hoffmeister asteroid family

Carruba

Novaković

Aljbaae

2016

Mon. Not. R. Astron. Soc.

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The Hoffmeister family is a C-type group located in the central main belt. Dynamically, it is important because of its interaction with the ν 1C nodal secular resonance with Ceres, that significantly increases the dispersion in inclination of family members at lower semi-major axis. As an effect, the distribution of inclination values of the Hoffmeister family at semi-major axis lower than its center is significantly leptokurtic, and this can be used to set constraints on the terminal ejection velocity field of the family at the time it was produced. By performing an analysis of the time behaviour of the kurtosis of the v W component of the ejection velocity field (γ 2 (v W )), as obtained from Gauss' equations, for different fictitious Hoffmeister families with different values of the ejection velocity field, we were able to exclude that the Hoffmeister family should be older than 335 Myr. Constraints from the currently observed inclination distribution of the Hoffmeister family suggest that its terminal ejection velocity parameter V EJ should be lower than 25 m/s. Results of a Yarko-YORP Monte Carlo method to family dating, combined with other constraints from inclinations and γ 2 (v W ), indicate that the Hoffmeister family should be 220

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Section: Physical Propertiesmentioning

confidence: 99%

“…We use the approach described in Carruba et al (2015a) that employs a Monte Carlo method (Vokrouhlický et al 2006a;Vokrouhlický et al 2006;Vokrouhlický et al 2006c) to estimate the age and terminal ejection velocities of the family members. More details on the method can be found in Carruba et al (2015a).…”

Section: Chronologymentioning

confidence: 99%

The Hoffmeister asteroid family

Carruba

Novaković

Aljbaae

2016

Mon. Not. R. Astron. Soc.

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“…At a 81.2% confidence level, the Erigone family should be 190 (Vokrouhlický et al 2006c, Bottke et al 2015, Spoto et al 2015.…”

Section: Discussionmentioning

confidence: 99%

On the Erigone family and thez₂secular resonance

Carruba

Aljbaae

Winter

2015

Mon. Not. R. Astron. Soc.

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The Erigone family is a C-type group in the inner main belt. Its age has been estimated by several researchers to be less then 300 My, so it is a relatively young cluster. Yarko-YORP Monte Carlo methods to study the chronology of the Erigone family confirm results obtained by other groups. The Erigone family, however, is also characterized by its interaction with the z 2 secular resonance. While less than 15% of its members are currently in librating states of this resonance, the number of objects, members of the dynamical group, in resonant states is high enough to allow to use the study of dynamics inside the z 2 resonance to set constraints on the family age.Like the ν 6 and z 1 secular resonances, the z 2 resonance is characterized by one stable equilibrium point at σ = 180• in the z 2 resonance plane (σ, dσ dt ), where σ is the resonant angle of the z 2 resonance. Diffusion in this plane occurs on timescales of ≃ 12 My, which sets a lower limit on the Erigone family age. Finally, the minimum time needed to reach a steady-state population of z 2 librators is about 90 My, which allows to impose another, independent constraint on the group age.

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“…It is also noteworthy that neither di Martino et al (1997) nor Zappala et al (1998) included the Yarkovsky effect in their simmulations, which could contribute to considerably shorten meteorite transport times (Bottke et al 2002, and references therein). Recently, Vokrouhlický et al (2005) developed a detailed theory of Yarkovsky evolution for the Eos family. This work suggests that drifting produced by the Yarkovsky effect could inject fragments into the 9/4 and 7/3 mean motion resonances, decreasing the transport times.…”

Section: Discussionmentioning

confidence: 99%

221 Eos: a remnant of a partially differentiated parent body?

Mothé-Diniz¹,

Carvano²

2005

A&A

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The asteroid 221 Eos and the objects belonging to its associated family -most of which belong to the K taxonomic class, have been traditionally associated with CO3/CV3 meteorites. The 52 color spectrum and the SMASSIR spectrum of 221 Eos in the NIR region, combined with the SMASSII spectrum in the visible, has now been compared to the whole RELAB meteorites database updated in July 2003. In this paper we present the first observational evidence that 221 Eos is analogous to a differentiated meteorite: the anomalous stone Divnoe. This link suggests that the the parent body of the Eos dynamical family was partially differentiated, with a thermal history quite different from what is currently accepted.

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The peculiar case of the Agnia asteroid family

Cited by 49 publications

References 47 publications

The Hoffmeister asteroid family

The Hoffmeister asteroid family

On the Erigone family and thez₂secular resonance

221 Eos: a remnant of a partially differentiated parent body?

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The peculiar case of the Agnia asteroid family

Cited by 49 publications

References 47 publications

The Hoffmeister asteroid family

The Hoffmeister asteroid family

On the Erigone family and thez2secular resonance

221 Eos: a remnant of a partially differentiated parent body?

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On the Erigone family and thez₂secular resonance