Non-linear secular resonances of g-type, i.e. involving the frequency of precession g of the asteroid pericentre, can affect the proper eccentricities of asteroids in resonant or near-resonant configurations. We first ...

Asteroid families are formed as the result of collisions. Large fragments are ejected with speeds of the order of the escape velocity from the parent body. After a family has been formed, the fragments' orbits evolve in ...

Nesta tese, nós introduzimos uma nova métrica no domínio dos elementos próprios, nas cores obtidas pela survey SDSS-MOC4 e nos albedos geométricos do WISE, com o objetivo de obter um método para determinar uma família ...

Among highly inclined asteroids the external region of the main belt beyond the 5J:2A mean-motion resonance with Jupiter has long been known to host the Euphrosyne and Alauda families. The region is confined in semimajor ...

Among highly inclined asteroids the external region of the main belt beyond the 5J:2A mean-motion resonance with Jupiter has long been known to host the Euphrosyne and Alauda families. The region is confined in semimajor ...

Asteroid families are groups of bodies identified in the space of proper elements or of frequencies that share a common origin in the collisional break-up of their progenitors. Their dynamical evolution is shaped by the ...

Asteroid families are groups of bodies identified in the space of proper elements or of frequencies that share a common origin in the collisional break-up of their progenitors. Their dynamical evolution is shaped by the ...

In a previous paper, the current state of knowledge on the region of the Pallas dynamical family was revised. Here the dynamical evolution and possible origin of dynamical groups in the region are investigated. First, we ...