Yarkovsky/YORP chronology of asteroid families

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

doi:10.1016/j.icarus.2005.12.010

Cited by 185 publications

(274 citation statements)

References 68 publications

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“…We tested the consistency between our "real" distribution and the theoretical one. We used a statistical approach similar to the usual χ 2 test, as for instance in Vokrouhlický et al (2006). The test parameter is defined as…”

Section: Taxonomy: Statistical Analysis Of Real Objectsmentioning

confidence: 99%

YORP effect on real objects

Micheli¹,

Paolicchi²

2008

A&A

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Context. The intensity of the YORP (Yarkovsky, O'Keefe, Radzievskii, and Paddack) effect and its ability to affect the rotational properties of asteroids depend mainly on the size of the body and on its shape. At present, we have a database of about 30 welldefined shapes of real minor bodies (most of them asteroids, but also planetary satellites and cometary nuclei). Aims. In this paper we perform a statistical analysis of how the YORP effect depends on the shape. Methods. We used the Rubincam approximation (i.e. neglecting the effects of a finite thermal conductivity). Results. We show that, among real bodies, the distribution of the YORP types, according to the classification of Vokrouhlický anď Capek, is significantly different from the one obtained in the same paper from theoretical modeling of shapes. A new "type" also comes out. Moreover, we show that the types are strongly correlated with the intensity of the YORP effect (when normalized to eliminate the dependence on the size, and thus only related to the shape).

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Section: Taxonomy: Statistical Analysis Of Real Objectsmentioning

confidence: 99%

YORP effect on real objects

Micheli¹,

Paolicchi²

2008

A&A

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“…3. One can also notice that, as for the case of the ν6 (Carruba and Morbidelli 2011) and z1 resonances (Vokrouhlický et al 2006b, Carruba 2009, there is an equilibrium point at σ = 180…”

Section: Dynamics Inside the Z2 Secular Resonancementioning

confidence: 83%

“…8, panel B, deals with conserved quantities of the z2 secular resonance. It is possible to show (see Carruba and Morbidelli 2011, Vokrouhlický et al 2006b, Carruba 2009, and calculations therein) that K2 ′ = √ 1 − e 2 (1 − cos i) is conserved for the ν6 resonance, K2 ′ = √ 1 − e 2 (2 − cos i) is preserved for the z1 resonance, and K2 ′ = √ 1 − e 2 (3 − cos i) is conserved for the z2 one. Fig.…”

Section: Dynamics Inside the Z2 Secular Resonancementioning

confidence: 92%

“…• , which corresponds to an uniform distribution of bodies along a circle (Vokrouhlický et al 2006b). This result suggests that any information about initial distributions of orbits inside the z2 resonance is lost very quickly, on a timescale of the order of 10 Myr.…”

Section: Dynamics Inside the Z2 Secular Resonancementioning

confidence: 99%

“…The z 2 secular resonance is a non-linear secular resonance that involves the combination of the two linear resonances ν 6 = g −g 6 and ν 16 = s−s 6 , of the z2 secular resonance. While this is not a majority of the members, as for the case of the Tina family and the ν6 secular resonance (100%, Carruba and Morbidelli 2011), the Agnia and Padua families, with more than 50% of the members in z1 librating states (Vokrouhlický et al 2006b, Carruba 2009), dynamics inside the z2 secular resonance can still be used to obtain estimates, or at least lower limits, of the family age.…”

Section: Introductionmentioning

confidence: 99%

See 2 more Smart Citations

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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