Physical parameters of selected Gaia mass asteroids
Authors:
- Edyta Podlewska-Gaca,
- Anna Marciniak,
- V. Alí-Lagoa,
- Przemysław Paweł Bartczak,
- T.G. Müller,
- R. Szakáts,
- R. Duffard,
- L. Molnár,
- A. Pál,
- Magda Butkiewicz-Bąk,
- Grzegorz Piotr Dudziński,
- Karolina Jadwiga Dziadura,
- P. Antonini,
- V. Asenjo,
- M. Audejean,
- Z. Benkhaldoun,
- R. Behrend,
- L. Bernasconi,
- J.M. Bosch,
- A. Chapman,
- B. Dintinjana,
- A. Farkas,
- M. Ferrais,
- S. Geier,
- J. Grice,
- Roman Hirsch,
- H. Jacquinot,
- E. Jehin,
- A. Jones,
- D. Molina,
- N. Morales,
- N. Parley,
- R. Poncy,
- R. Roy,
- Antonio Santana-Ros,
- B. Seli,
- K. Sobkowiak,
- E. Verebélyi,
- Kamil Żukowski
Abstract
Context. Thanks to the Gaia mission, it will be possible to determine the masses of approximately hundreds of large main belt asteroids with very good precision. We currently have diameter estimates for all of them that can be used to compute their volume and hence their density. However, some of those diameters are still based on simple thermal models, which can occasionally lead to volume uncertainties as high as 20-30%. Aims. The aim of this paper is to determine the 3D shape models and compute the volumes for 13 main belt asteroids that were selected from those targets for which Gaia will provide the mass with an accuracy of better than 10%. Methods. We used the genetic Shaping Asteroids with Genetic Evolution (SAGE) algorithm to fit disk-integrated, dense photometric lightcurves and obtain detailed asteroid shape models. These models were scaled by fitting them to available stellar occultation and/or thermal infrared observations. Results. We determine the spin and shape models for 13 main belt asteroids using the SAGE algorithm. Occultation fitting enables us to confirm main shape features and the spin state, while thermophysical modeling leads to more precise diameters as well as estimates of thermal inertia values. Conclusions. We calculated the volume of our sample of main-belt asteroids for which the Gaia satellite will provide precise mass determinations. From our volumes, it will then be possible to more accurately compute the bulk density, which is a fundamental physical property needed to understand the formation and evolution processes of small Solar System bodies.
- Record ID
- UAM07f30dd540a04b83859d5f73ee3c9ea5
- Author
- Journal series
- Astronomy & Astrophysics, ISSN 0004-6361, e-ISSN 1432-0746
- Issue year
- 2020
- Vol
- 638
- Article number
- A11
- ASJC Classification
- ;
- DOI
- DOI:10.1051/0004-6361/201936380 Opening in a new tab
- Language
- (en) English
- Score (nominal)
- 140
- Score source
- journalList
- Score
- = 140.0, 18-05-2022, ArticleFromJournal
- Publication indicators
- = 3; = 2; = 5; : 2018 = 1.233; : 2019 (2 years) = 5.636 - 2019 (5 years) =5.395
- Citation count
- 6
Share
- Uniform Resource Identifier
- https://researchportal.amu.edu.pl/info/article/UAM07f30dd540a04b83859d5f73ee3c9ea5/
- URN
urn:amu-prod:UAM07f30dd540a04b83859d5f73ee3c9ea5
* presented citation count is obtained through Internet information analysis and it is close to the number calculated by the Publish or PerishOpening in a new tab system.