Valerio Carruba

• Abstract

  Asteroid families are groups of objects that have similar orbits. They can be produced as the result of a collision between a projectile andthe family parent body (collisional families), or because of the fission of a secondary body or of a low-energy impact on a rapidly rotating primary(fission clusters). Collisional families tend to be more dispersed in semi-major axis and they are usua…

  Young asteroid families: exploring the limit between fission groups and collisional families, AP.R

• Abstract

  Asteroid families form as a result of large-scale collisions among main belt asteroids. The orbital distribution of fragments after a family-forming impact could inform us about their ejection velocities. Unfortunately, however, orbits dynamically evolve by a number of effects, including the Yarkovsky drift, chaotic diffusion, and gravitational encounters with massive asteroids, such tha…

  Constraints on the terminal ejection velocity fields of asteroid families, AP.R

• Abstract

  Euphrosyne is the largest body of its namesake family and it contains more then 99% of the family mass. Among large asteroid families, the Euphrosyne group is peculiar because of its quite steep size frequency distribution, significantly depleted in large and medium-sized asteroids (8 < D < 12 km).The current steep size frequency distribution of the Euphrosyne family has been suggested to…

  Peculiar Euphrosyne, PUB.ART

(Only some records are available in English at this moment)

• Abstract

  Carruba et al. (2013a) studied the long-term effect of close encounters with massive asteroids for asteroids in the orbital region of the Hygiea, Euphrosyne, and Pallas families. Since changes in heliocentric velocities that cause changes in proper elements are a function of the minimal velocity and distance at the encounter, it was shown analytically and numerically that the robustness …

  Long-term effect of the masses (and their uncertainties) of large asteroids on the orbital evolution of terrestrial planetes and minor bodies., BP.PD

• Abstract

  Among the largest asteroids in the main belt, asteroid 4 Vesta is unique in showing a basaltic crust. It is also the biggest member of the Vesta family, which is supposed to originate from a large cratering event about 1 Gyr ago (Marzari et al. 1996, Carruba et al. 2005). Most of the members of the Vesta family for which a spectral classification is available show a V-type spectra. Due to…

  Dynamics and origin of asteroid families., BP.JP

• Abstract

  The current structure of the Solar System was deeply shaped by the effects of planetary migration. The most recent models of planetary migration suggest that the current orbital distribution of asteroids, and in particular the low ratio between highly and low inclined population could be better explained in the ``Jumping-Jupiter'' scenario, in which both Jupiter and Saturn have close enco…

  Dynamical evolution of asteroid families, BE.PQ