Short-lived asteroids in the 7/3 Kirkwood gap and their relationship to the Koronis and Eos families

Tsiganis, K.; Varvoglis, H.; Morbidelli, Alessandro

doi:10.1016/j.icarus.2003.08.007

Cited by 34 publications

(36 citation statements)

References 14 publications

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“…This result agrees with what numerical integrations show, i.e. test-particles may take more than 1 Gyr to leave a high-order resonance (Tsiganis, Varvoglis & Hadjidemetriou (2002b), Tsiganis & Morbidelli (2003)). …”

Section: Diffusion Of Asteroids -Mathematical Formulationsupporting

confidence: 91%

Diffusion in the asteroid belt

Varvoglis

2004

Proc. IAU

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Abstract. In the beginning we review briefly the evolution of the ideas on the motion of the bodies in our solar system, from Newton's clockwork Universe to the presently accepted ubiquity of chaotic transport in the asteroid belt. Then we discuss the result of chaotic motion, which is transport in phase space, and we introduce the concept of diffusion of an asteroid in action space. We proceed by reviewing recent work on numerical as well as analytical study of asteroids following chaotic trajectories and we summarize the main results. We present several applications of the theoretical modelling of asteroid motion as diffusion in action space, to problems of specific interest.

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Section: Diffusion Of Asteroids -Mathematical Formulationsupporting

confidence: 91%

Diffusion in the asteroid belt

Varvoglis

2004

Proc. IAU

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“…For a comparison the present inclination of 2001 XR31 is 22.7 deg. Notice that, the dynamical behavior of such fragments would be quite similar to that of Eos-like objects which have been investigated recently by Tsiganis et al (2003). They found a mean resident-time in the 7:3 of 12.4 Myr, and that such Eos-like objects can reach inclination of about 16 deg, before being ejected from the resonance by close encounter with Jupiter.…”

Section: Dynamical Implicationssupporting

confidence: 61%

“…The variation of the inclination due to the evolution driven by the resonances alone can be of a few degree at most (see Fig. 3b in Tsiganis et al 2003;Yoshikawa 1989). A similar increase in inclination can probably also be achieved by close encounters with Earth and/or Venus, as shown for the Alinda class by Milani et al (1989).…”

Section: Dynamical Implicationsmentioning

confidence: 99%

An R-type asteroid within near-Earth objects?

Marchi

Lazzarin

Magrin

2004

A&A

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Abstract. We present visible and near-infrared spectroscopy of 2001 XR31, a previously unclassified small near-Earth object (NEOs). Its spectrum resembles that of basaltic body, with the distinctive 1 and 2 µm pyroxene absorption bands, similar to those found on V-type bodies. However, the spectrum of 2001 XR31 is somewhat peculiar and we discuss whether it can belong to another class of basaltic bodies, namely the rare R-class. If confirmed, this object would be the only R-type detected among NEOs so far. In the light of this possibility, we also discuss the relationships of 2001 XR31 with other main belt R-types and a possible explanation of its origin.

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“…P/2006 VW 139 itself is found to be stable over the 100 Myr test period (neglecting non-gravitational forces), consistent with its Lyapunov time of T lyap > 1 Myr, where a body is considered stable if T lyap > 100 kyr (Tsiganis et al 2003). No systematic distribution is evident for ejected 1σ or 10σ test particles, though 44% of 100σ test particles with a < 3.04 AU are ejected, perhaps due to the 9J:4A mean-motion resonance with Jupiter at 3.029 AU (Figure 4(b)).…”

Section: Dynamical Analysismentioning

confidence: 55%

DISCOVERY OF MAIN-BELT COMET P/2006 VW₁₃₉BY Pan-STARRS1

Hsieh

Yang

Haghighipour

et al. 2012

ApJ

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The main-belt asteroid (300163) 2006 VW 139 (later designated P/2006 VW 139 ) was discovered to exhibit comet-like activity by the Pan-STARRS1 (PS1) survey telescope using automated point-spread-function analyses performed by PS1's Moving Object Processing System. Deep follow-up observations show both a short (∼10 ) antisolar dust tail and a longer (∼60 ) dust trail aligned with the object's orbit plane, similar to the morphology observed for another main-belt comet (MBC), P/2010 R2 (La Sagra), and other well-established comets, implying the action of a long-lived, sublimation-driven emission event. Photometry showing the brightness of the near-nucleus coma remaining constant over ∼30 days provides further evidence for this object's cometary nature, suggesting it is in fact an MBC, and not a disrupted asteroid. A spectroscopic search for CN emission was unsuccessful, though we find an upper limit CN production rate of Q CN < 1.3 × 10 24 mol s −1 , from which we infer a water production rate of Q H 2 O < 10 26 mol s −1 . We also find an approximately linear optical spectral slope of 7.2%/1000 Å, similar to other cometary dust comae. Numerical simulations indicate that P/2006 VW 139 is dynamically stable for >100 Myr, while a search for a potential asteroid family around the object reveals a cluster of 24 asteroids within a cutoff distance of 68 m s −1 . At 70 m s −1 , this cluster merges with the Themis family, suggesting that it could be similar to the Beagle family to which another MBC, 133P/Elst-Pizarro, belongs.

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Short-lived asteroids in the 7/3 Kirkwood gap and their relationship to the Koronis and Eos families

Cited by 34 publications

References 14 publications

Diffusion in the asteroid belt

Diffusion in the asteroid belt

An R-type asteroid within near-Earth objects?

DISCOVERY OF MAIN-BELT COMET P/2006 VW₁₃₉BY Pan-STARRS1

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Short-lived asteroids in the 7/3 Kirkwood gap and their relationship to the Koronis and Eos families

Cited by 34 publications

References 14 publications

Diffusion in the asteroid belt

Diffusion in the asteroid belt

An R-type asteroid within near-Earth objects?

DISCOVERY OF MAIN-BELT COMET P/2006 VW139BY Pan-STARRS1

Contact Info

Product

Resources

About

DISCOVERY OF MAIN-BELT COMET P/2006 VW₁₃₉BY Pan-STARRS1