Evolution of an Asteroid Family under YORP, Yarkovsky, and Collisions

  title={Evolution of an Asteroid Family under YORP, Yarkovsky, and Collisions},
  author={Francesco Marzari and Alessandro Rossi and Oleksiy Golubov and Daniel J. Scheeres},
  journal={arXiv: Earth and Planetary Astrophysics},
Any population of asteroids, like asteroid families, will disperse in semi-major axis due to the Yarkovsky effect. The amount of drift is modulated by the asteroid spin state evolution which determines the balance between the diurnal and seasonal Yarkovsky force. The asteroid's spin state is, in turn, controlled in part by the YORP effect. The otherwise smooth evolution of an asteroid can be abruptly altered by collisions, which can cause impulsive changes in the spin state and can move the… 
Limiting Behavior of Asteroid Obliquity and Spin Using a Semi-analytic Thermal Model of the YORP Effect
The Yarkovsky–O’Keefe–Radzievskii–Paddack (YORP) effect governs the spin evolution of small asteroids. The axial component of YORP, which alters the rotation rate of the asteroid, is mostly
The impact of physical processes on the estimation of the ages of asteroid families
One of the methods used to estimate the ages of the asteroid families is based on the interpretation of the distribution of the sizes versus orbital semimajor axes of their members as the result of
Dynamical constraints on the evolution of the inner asteroid belt and the sources of meteorites
Abstract We have shown that in the inner belt the loss of asteroids from the ν6 secular resonance and the 3:1 Jovian mean motion resonance accounts for the observation that the mean size of the
Asteroid Families: properties, recent advances and future opportunities
Collisions are one of the key processes shaping planetary systems. Asteroid families are outcomes of such collision still identifiable across our solar system. The families provide a unique view of
Mercury and orbfit packages for numerical integration of planetary systems: implementation of the yarkovsky and yorp effects
For studies of the long-term evolution of small Solar System objects, it is fundamental to add the Yarkovsky and Yarkovsky-O'Keefe-Radzievskii-Paddack (YORP) effects in the dynamical model. Still,
Using Mars co-orbitals to estimate the importance of rotation-induced YORP break-up events in Earth co-orbital space
Both Earth and Mars host populations of co-orbital minor bodies. A large number of presentday Mars co-orbitals is probably associated with the fission of the parent body of Mars Trojan 5261 Eureka


Footprints of the YORP effect in asteroid families
Combined effect of YORP and collisions on the rotation rate of small Main Belt asteroids
Systematic Structure and Sinks in the YORP Effect
There is a correlation between the components of the YORP effect of most asteroids, which drives the obliquity and spin rate of the affected bodies in a consistent pattern. This allows for a clear
Dynamical Spreading of Asteroid Families by the Yarkovsky Effect
Assuming that D ≲ 20 kilometer family members, since their formation, have undergone semimajor axis drift by the thermal force called the Yarkovsky effect helps explain why families are sharply bounded by nearby Kirkwood gaps, why some families have asymmetric shapes, and the curious presence of family members on short-lived orbits.
Asteroid orbit evolution due to thermal drag
Thermal drag, a variant of the Yarkovsky effect, may act on small asteroids with sizes from a few meters to a few tens of meters. Yarkovsky thermal drag comes from an asteroid's absorbing sunlight in
The Yarkovsky and YORP Effects
The Yarkovsky effect describes a small but significant force that affects the orbital motion of meteoroids and asteroids smaller than $30-40$ kilometers in diameter. It is caused by sunlight; when
The recent breakup of an asteroid in the main-belt region
The discovery of a family of asteroids that formed in a disruption event only 5.8 ± 0.2 million years ago, and which has subsequently undergone little dynamical and collisional evolution, is reported.
Near Earth Asteroids with measurable Yarkovsky effect
Ages of asteroid families estimated using the YORP-eye method
Recently, we have shown that it is possible, despite several biases and uncertainties, to find footprints of the Yarkovsky–O’Keefe–Radzievskii–Paddack (YORP) effect, concerning the members of