Spin states of asteroids in the Eos collisional family

@article{Hanuvs2018SpinSO,
  title={Spin states of asteroids in the Eos collisional family},
  author={Josef Hanuvs and Marco Delbo’ and V'ictor Al'i-Lagoa and Bryce T. Bolin and Robert Jedicke and Josef vDurech and Helena Cibulkov'a and Petr Pravec and Peter Kuvsnir'ak and Raoul Behrend and Franck Marchis and P. Antonini and L. A. Arnold and Maurice Audejean and Matthieu Bachschmidt and Laurent Bernasconi and L. Brunetto and Silvano Casulli and Roger Dymock and N. Esseiva and Mar{\'i}a Dolores P{\'e}rez Esteban and O. Gerteis and Holger de Groot and H. Gully and Hiromi Hamanowa and P. Krafft and Martin Lehk'y and Federico Manzini and J. Michelet and Etienne Morelle and Julian Oey and Frederick Pilcher and F. Reignier and R. Roy and P. A. Salom and Brian D. Warner},
  journal={Icarus},
  year={2018},
  volume={299},
  pages={84-96}
}

Figures and Tables from this paper

Inversion of asteroid photometry from Gaia DR2 and the Lowell Observatory photometric database

Context. Rotation properties (spin-axis direction and rotation period) and coarse shape models of asteroids can be reconstructed from their disk-integrated brightness when measured from various

Asteroid models reconstructed from the Lowell Photometric Database and WISE data

Context. Information about the spin state of asteroids is important for our understanding of the dynamical processes affecting them. However, spin properties of asteroids are known for only a small

Asteroid migration due to the Yarkovsky effect and the distribution of the Eos family

Based on a linearized model of the Yarkovsky effect, we investigate in this paper the dependence of the semimajor axis drift $\Delta a$ of a celestial body on its size, spinning obliquity, initial

A study of 3-dimensional shapes of asteroid families with an application to Eos

In order to fully understand the shapes of asteroids families in the 3-dimensional space of the proper elements (ap, ep, sin Ip) it is necessary to compare observed asteroids with N-body simulations.

Dynamical evolution of the inner asteroid belt

  • S. DermottDan Li UK.
  • Physics, Geology
    Monthly Notices of the Royal Astronomical Society
  • 2020
A determination of the dynamical evolution of the asteroid belt is difficult because the asteroid belt has evolved since the time of asteroid formation through mechanisms that include: (1)

Thermal properties of slowly rotating asteroids: results from a targeted survey

Context. Earlier work suggests that slowly rotating asteroids should have higher thermal inertias than faster rotators because the heat wave penetrates deeper into the subsurface. However, thermal

Thermal Properties of 1847 WISE-observed Asteroids

We present new thermophysical model fits of 1847 asteroids, deriving thermal inertia, diameter, and Bond and visible geometric albedo. We use thermal flux measurements obtained by the Wide-field

Thermal properties of large main-belt asteroids observed by Herschel PACS

Non-resolved thermal infrared observations enable studies of thermal and physical properties of asteroids via thermo-physical models provided the shape and rotational properties of the target are

References

SHOWING 1-10 OF 105 REFERENCES

An anisotropic distribution of spin vectors in asteroid families

Current amount of ~500 asteroid models derived from the disk-integrated photometry by the lightcurve inversion method allows us to study not only the spin-vector properties of the whole population of

ROTATIONAL PROPERTIES OF THE MARIA ASTEROID FAMILY

The Maria family is regarded as an old-type (∼3 ± 1 Gyr) asteroid family that has experienced substantial collisional and dynamical evolution in the main belt. It is located near the 3:1 Jupiter

The Eos family halo

Spin vector alignment of Koronis family asteroids

Reconciling models of family formation and evolution with the unexpected alignments of spin obliquities and correlations with spin rates presents a new challenge in understanding asteroid collisional processes.

Asteroid family ages

Asteroid Models from Multiple Data Sources

In the past decade, hundreds of asteroid shape models have been derived using the lightcurve inversion method. At the same time, a new framework of 3-D shape modeling based on the combined analysis

Asteroids’ physical models from combined dense and sparse photometry and scaling of the YORP effect by the observed obliquity distribution

The larger number of models of asteroid shapes and their rotational states derived by the lightcurve inversion give us better insight into both the nature of individual objects and the whole asteroid
...