The depletion of objects in the central part of an asteroid family, which can be observed in the absolute magnitude vs. semimajor axis, can be explained in terms of a coupling of the YORP and Yarkovsky effects (Paolicchi and Knezevic, Icarus, 2016). In particular, it can be ascribed to the obliquity evolution caused by YORP and on how it influences the Yarkovsky drift. Exploiting the recent work by Golubov & Scheeres, a more accurate treatment of the coupling between the obliquity and spin rate evolution was introduced in a model which tracks the evolution of the spin vector of small asteroids, including also the effects of collisions on the YORP induced obliquity evolution. Considering a few model families and simulating their time evolution in the magnitude vs. semimajor axis plots, the model is being validated and the YORP-eye hypothesis in presence of collisional activity is tested.
Effects of collisions on the YORP-Yarkovsky evolution of asteroid families
A Rossi;
2018
Abstract
The depletion of objects in the central part of an asteroid family, which can be observed in the absolute magnitude vs. semimajor axis, can be explained in terms of a coupling of the YORP and Yarkovsky effects (Paolicchi and Knezevic, Icarus, 2016). In particular, it can be ascribed to the obliquity evolution caused by YORP and on how it influences the Yarkovsky drift. Exploiting the recent work by Golubov & Scheeres, a more accurate treatment of the coupling between the obliquity and spin rate evolution was introduced in a model which tracks the evolution of the spin vector of small asteroids, including also the effects of collisions on the YORP induced obliquity evolution. Considering a few model families and simulating their time evolution in the magnitude vs. semimajor axis plots, the model is being validated and the YORP-eye hypothesis in presence of collisional activity is tested.I documenti in IRIS sono protetti da copyright e tutti i diritti sono riservati, salvo diversa indicazione.
