Statistical evidence for fast and slow asteroid rotations using Bayesian methods

Donnison, J. R.

doi:10.1046/j.1365-8711.2003.06064.x

Cited by 4 publications

(3 citation statements)

References 22 publications

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“…2 2 According to Paolicchi, Verlicchi & Cellino (1996), a size–rotation relation suggests that smaller fragments are rotating somewhat faster than the larger ones (see also Donnison 2003). Also, Kryszczyńska et al (2007) claim that the poles are not isotropically distributed, as general theoretical considerations may predict.…”

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confidence: 99%

Chaotic transport and chronology of complex asteroid families

Novaković

Tsiganis

Knežević

2010

Monthly Notices of the Royal Astronomical Society

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We present a transport model that describes the orbital diffusion of asteroids in chaotic regions of the three-dimensional space of proper elements. Our goal is to use a simple random-walk model to study the evolution and derive accurate age estimates for dynamically complex asteroid families. To this purpose, we first compute local diffusion coefficients, which characterize chaotic diffusion in proper eccentricity (e p ) and inclination (I p ), in a selected phase-space region. Then, a Monte Carlo type code is constructed and used to track the evolution of random walkers (i.e. asteroids), by coupling diffusion in (e p , I p ) with a drift in proper semimajor axis (a p ) induced by the Yarkovsky/YORP thermal effects. We validate our model by applying it to the family of (490) Veritas, for which we recover previous estimates of its age (∼8.3 Myr). Moreover, we show that the spreading of chaotic family members in proper element space is well reproduced in our random-walk simulations. Finally, we apply our model to the family of (3556) Lixiaohua, which is much older than Veritas and thus much more affected by thermal forces. We find the age of the Lixiaohua family to be 155 ± 36 Myr.

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confidence: 99%

Chaotic transport and chronology of complex asteroid families

Novaković

Tsiganis

Knežević

2010

Monthly Notices of the Royal Astronomical Society

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“…Are collisions likely to damage asteroids? Well, the four that have been imaged so far have the distributions of crater sizes you would expect (Jeffers & Asher 2003), but the distribution of rotation periods (hours to days is typical) suggests that major collisions are not very common (Donnison 2003;Vokrouhlicky et al 2003).…”

Section: Little Starsmentioning

confidence: 99%

Astrophysics in 2003

Trimble

Aschwanden

2004

PUBL ASTRON SOC PAC

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Five coherent sections appear this year, addressing solar physics, cosmology (with WMAP highlights), gamma-ray bursters (and their association with Type Ia supernovae), extra-solar-system planets, and the formation and evolution of galaxies (from reionization to assemblage of Local Group galaxies). There are also eight incoherent sections that deal with other topics in stellar, galactic, and planetary astronomy and the people who study them. INTRODUCTIONSTriskaidekaphobics may prefer not to read this installment of ApXX, and their numbers may well be augmented even before the introduction is over. This is, in fact, the 13th overview of 365.24 days of the astronomy and astrophysics literature. The earlier ones are cited here as Ap91, Ap92, …, Ap02 and appear in volumes 104-115 of PASP. The authors have tried to read systematically the contents of about 30 journals and other periodicals. Only about 10% of what has been read gets cited, and being cited is not always an unqualified compliment.Section 2 was assembled using papers found on the Astrophysics Data Service, maintained with support from NASA and including Solar

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“…According toPaolicchi et al (1996) a size-rotation relation suggests that smaller fragments are rotating somewhat faster than the larger ones (see alsoDonnison 2003). Also,Kryszczyńska et al (2007) claim that the poles are not isotropically distributed, as general theoretical considerations may predict.…”

mentioning

confidence: 96%

Chaotic Transport and Chronology of Complex Asteroid Families

Novakovic,

Tsiganis,

Knezevic

2009

Preprint

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We present a transport model that describes the orbital diffusion of asteroids in chaotic regions of the 3-D space of proper elements. Our goal is to use a simple random-walk model to study the evolution and derive accurate age estimates for dynamically complex asteroid families. To this purpose, we first compute local diffusion coefficients, which characterize chaotic diffusion in proper eccentricity (e p ) and inclination (I p ), in a selected phase-space region. Then, a Monte-Carlo-type code is constructed and used to track the evolution of random walkers (i.e. asteroids), by coupling diffusion in (e p ,I p ) with a drift in proper semi-major axis (a p ) induced by the Yarkovsky/YORP thermal effects. We validate our model by applying it to the family of (490) Veritas, for which we recover previous estimates of its age (∼ 8.3 Myr). Moreover, we show that the spreading of chaotic family members in proper elements space is well reproduced in our randomk-walk simulations. Finally, we apply our model to the family of (3556) Lixiaohua, which is much older than Veritas and thus much more affected by thermal forces. We find the age of the Lixiaohua family to be 155 ± 36 Myr.

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Statistical evidence for fast and slow asteroid rotations using Bayesian methods

Cited by 4 publications

References 22 publications

Chaotic transport and chronology of complex asteroid families

Chaotic transport and chronology of complex asteroid families

Astrophysics in 2003

Chaotic Transport and Chronology of Complex Asteroid Families

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