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Register a new userAsteroid triple system 2001 SN263 : surfaces characteristics and dynamical environment
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The (153591) 2001 SN263 asteroid system, target of the first Brazilian interplanetary space mission, is one of the known three triple systems within the population of NEAs. One of the mission objectives is to collect data about the formation of this system. The analysis of these data will help in the investigation of the physical and dynamical structures of the components (Alpha, Beta and Gamma) of this system, in order to find vestiges related to its origin. In this work, we assume the irregular shape of the 2001 SN263 system components as uniform density polyhedra and computationally investigate the gravitational field generated by these bodies. The goal is to explore the dynamical characteristics of the surface and environment around each component. Then, taking into account the rotational speed, we analyze their topographic features through the quantities geometric altitude, tilt, geopotential, slope, surface accelerations, among others. Additionally, the investigation of the environment around the bodies made it possible to construct zero-velocity curves, which delimit the location of equilibrium points. The Alpha component has a peculiar number of 12 equilibrium points, all of them located very close to its surface. In the cases of Beta and Gamma, we found four equilibrium points not so close to their surfaces. Then, performing numerical experiments around their equilibrium points, we identified the location and size of just one stable region, which is associated with an equilibrium point around Beta. Finally, we integrated a spherical cloud of particles around Alpha and identified the location on the surface of Alpha were the particles have fallen.
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From a set of adaptive optics (AO) observations collected with the W.M. Keck telescope between August and September 2009, we derived the orbital parameters of the most recently discovered satellites of the large C-type asteroid (93) Minerva. The satellites of Minerva, which are approximately 3 and 4 km in diameter, orbit very close to the primary $sim$5 & $sim$8 $times$ Rp and $sim$1% & $sim$2% $times$ RHill) in a circular manner, sharing common characteristics with most of the triple asteroid systems in the main-belt. Combining these AO observations with lightcurve data collected since 1980 and two stellar occultations in 2010 & 2011, we removed the ambiguity of the pole solution of Minervas primary and showed that it has an almost regular shape with an equivalent diameter Deq = 154 $pm$ 6 km in agreement with IRAS observations. The surprisingly high bulk density of 1.75 $pm$ 0.30 g/cm$^3$ for this C-type asteroid, suggests that this taxonomic class is composed of asteroids with different compositions, For instance, Minerva could be made of the same material as dry CR, CO, and CV meteorites. We discuss possible scenarios on the origin of the system and conclude that future observations may shine light on the nature and composition of this fifth known triple main-belt asteroid.
In this paper we present results of our studying of famous very young pair of asteroids 6070 Rheinland and 54827 (2001 NQ8). We have done numeric integration of orbits of pair with only planet perturbations and include Ceres and Vesta effect. We have confirmed results of previous studying, obtained with different integrators. And we confirm significant effect of Ceres and Vesta perturbation on dynamic of this pair. We find that effect of other massive asteroids is insignificant. According our results, more probable age of 6070 Rheinland and 54827 (2001 NQ8) pair is 16.2 kyrs. Our value of age is very close to most recent age determination by Vokrouhlicky et al [12], obtained with different method. After the compare our results, we can conclude, that non-gravitational forces are small and large number of clones is not necessary in studying of this pair. As an additional way of studying of close orbits dynamics, we calculate relative velocity in pair during numeric integration. Normal component of velocity show a very good convergence at epoch of closest encounter in pair.
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