SIMBAD references

2017AcA....67...81W - Acta Astron., 67, 81-102 (2017/January-0)

Discovery, Orbit and Orbital Evolution of the Distant Object (463368) 2012 VU85.

WLODARCZYK I., CERNIS K. and BOYLE R.P.

Abstract (from CDS):

We present the discovery and time evolution of orbital elements of the distant Centaur-type object (463368) 2012 VU85. From all 2135 distant objects listed in the Minor Planet Center we select all 347 numbered distant object and integrate their equations of motion in the 1 Gyr forward and backward integration. The asteroid (463368) 2012 VU85 lies on the border of the group of 347 distant objects, which have a semimajor axis about 44 a.u., eccentricity 0.1 and inclination between 0° and 30°. We show that after 1 Gyr of forward integration, about half of the objects are expelled from the Solar System, \ie their median lifetime is about 1 Gyr. We note that the long-lived distant objects are mainly located between the regions where Neptune controls aphelia of asteroids and the asteroids are in the mean motion resonance 2/3 with Neptune. We find eight almost regular approaches of clones of the asteroid (463368) 2012 VU85 to Neptune and several generally shorter in time regular approaches to Uranus. For other outer planets we did not detect any approaches below 5 a.u. for a period of 15 000 yr in forward and backward integrations. In our calculations we find eight episodes, each lasting about 3000 yr when the value of inclination oscillates around its average. These changes look similar to the changes of semimajor axis during the occurrence of orbital mean motion resonance with a planet. We find that half of the clones of the asteroid (463368) 2012 VU85 remain in the Solar System for a forward integration of 44 Myr, and for a backward integration of 34 Myr. This is a significantly shorter escape time as compared to the group of distant objects. Almost all long-lived clones have value of Tisserand parameter with respect to Neptune smaller than 3 during the whole 1 Gyr forward and backward integrations. This implies that there are several clones of the asteroid (463368) 2012 VU85 that cross the orbits of Neptune and Uranus. We find many orbital mean motion resonances lasting up to several Myr in the motion of the asteroid (463368) 2012 VU85. According to our computations the presence of the Kozai resonance protects the asteroid from the close approaches with Uranus and Neptune. The Lyapunov time for the asteroid (463368) 2012 VU85 is equal to 4260 years.

Abstract Copyright:

Journal keyword(s): Minor planets: asteroids: individual: (463368) 2012 VU85

Simbad objects: 3

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2019.12.14-15:17:58

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