Forward orbital evolution of the Vesta Family with and without the Yarkovsky effect

Vesta Family Members (VFMs) were identified by means of the Hierarchical Clustering Method (HCM). More precisely the HCM only allows to identify the VFMs-candidates. However, some of the candidates could be the interlopers that are not genetically related to the family. Farther on we treat all 17164 asteroids chosen by HCM as the VFMs. It is well known that the Yarkovsky Effect (YE) influences orbits of small bodies of the Solar System, particularly the orbits of asteroids. The goal of this work is comparing evolution of the Vesta Family (VF) without the Yar kovsky effect (YN) with their evolution when the YE is considered (YY) . In fact it is not so important to consider all selected asteroids as the real VFMs or only as the potential VFMs that are as the real ones admixed by interlopers. Essential is a study of orbital evolution of a large set of asteroids following two different models. So, in this paper no effort is done to eliminate interlopers. We use an abbreviated form VFMs instead of the correct form VFMs-candidates. Orbital evolution, that is the changes ∆a, ∆e, and ∆i of semiaxis a, of eccentricity e, and of orbital inclination i vs time is studied for all 17164 asteroids identified as VFMs. Orbital evolution of them is performed 1 Gy forward. Numerical algorithm is organized in such a manner that an access is granted to partial results, i.e. to the instantaneous values of orbital parameters of the all asteroids considered in each moment of orbital integration.