| Full text | |
| Author(s): |
Carruba, V.
Total Authors: 1
|
| Document type: | Journal article |
| Source: | Planetary and Space Science; v. 166, p. 90-100, FEB 2019. |
| Web of Science Citations: | 0 |
| Abstract | |
The Beagle family is a C-type subgroup of the Themis family, in the outer main belt. Previous works suggested that it could be younger than 20 Myr and a possible source for the dust in the i similar or equal to 1.4 degrees alpha zodiacal dust band. Here we took advantage of a much larger database for Beagle family members to revisit previous age estimates of this group. Standard dating techniques based on the family V-shape or on Monte Carlo methods of Yarkovsky and YORP mobility suggest that i) there might be a dichotomy for the inner and outer part of the Beagle family, which may be either two separate families or the product of an anisotropic ejection velocity field and that ii) the age of the possibly younger outer part of the Beagle family should be 35(-35)(+65) Myr. The past convergence of Beagle longitude of the node is compatible with a family age of similar or equal to 14 Myr, when (1678) Glarona is used as a reference orbit. Without further information on Beagle members spin states, however, only very lower limits on the family age can be currently obtained when the Yarkovksy force is accounted for. (AU) | |
| FAPESP's process: | 16/04476-8 - Constraints on the terminal ejection velocity fields of asteroid families |
| Grantee: | Valerio Carruba |
| Support Opportunities: | Regular Research Grants |