Internal structure of asteroid gravitational aggregates

Por favor, use este identificador para citar o enlazar este ítem: http://hdl.handle.net/10045/71837
Información del item - Informació de l'item - Item information
Título: Internal structure of asteroid gravitational aggregates
Autor/es: Campo Bagatin, Adriano | Alemañ Berenguer, Rafael Andrés | Benavídez, Paula Gabriela | Richardson, Derek C.
Grupo/s de investigación o GITE: Astronomía y Astrofísica
Centro, Departamento o Servicio: Universidad de Alicante. Departamento de Física, Ingeniería de Sistemas y Teoría de la Señal | Universidad de Alicante. Instituto Universitario de Física Aplicada a las Ciencias y las Tecnologías
Palabras clave: Asteroids | Interiors | Collisional physics
Área/s de conocimiento: Física Aplicada
Fecha de publicación: 1-mar-2018
Editor: Elsevier
Cita bibliográfica: Icarus. 2018, 302: 343-359. doi:10.1016/j.icarus.2017.11.024
Resumen: The internal structure of small asteroids is fundamentally unknown due to lack of direct measurements. The only clues on this topic come from theoretical considerations and from the comparison between measured bulk densities of asteroids and their corresponding analogue meteorite densities. The mass distribution and the void space between components in a gravitational aggregate determine the structure of such objects. In this paper we study numerically the dynamical and collisional evolution of the reaccumulation process of the fragments created in catastrophic collisions of asteroids in the 500 m to 10 km size range. An effort to consider irregularly shaped fragments is made by taking advantage of the results of laboratory experiments that provide relative mass distributions and aspect ratios for fragment shapes. We find that the processes that govern the final properties of the resulting aggregates are mainly stochastic, however interesting patterns can be identified. This study matches estimated macro-porosities of S-type asteroids and finds a loose linear relationship between macro-prorosity of asteroid aggregates and the mass ratio of the largest component to the whole aggregate (for both S and C-types). As for observed C-type asteroids, we conclude that their interiors should be more fragmented than in the case of S-type asteroids, explaining the difference in the estimated macro-porosity of real C asteroids with respect to S-types. We also find that slow rotators may be interpreted as a natural result in the process of gravitational reaccumulation.
Patrocinador/es: This work has been possible thanks to the grants AYA2008- 06202C0303 and AYA2011-30106-C02-02 by the extinct Spanish Ministerio de Ciencia e Innovación.
URI: http://hdl.handle.net/10045/71837
ISSN: 0019-1035 (Print) | 1090-2643 (Online)
DOI: 10.1016/j.icarus.2017.11.024
Idioma: eng
Tipo: info:eu-repo/semantics/article
Derechos: © 2017 Elsevier Inc.
Revisión científica: si
Versión del editor: http://dx.doi.org/10.1016/j.icarus.2017.11.024
Aparece en las colecciones:INV - Astronomía y Astrofísica - Artículos de Revistas

Archivos en este ítem:
Archivos en este ítem:
Archivo Descripción TamañoFormato 
Thumbnail2018_Campo-Bagatin_etal_Icarus_final.pdfVersión final (acceso restringido)1,3 MBAdobe PDFAbrir    Solicitar una copia
Thumbnail2018_Campo-Bagatin_etal_Icarus_accepted.pdfEmbargo 24 meses (acceso abierto: 23 nov. 2019)1,1 MBAdobe PDFAbrir    Solicitar una copia


Todos los documentos en RUA están protegidos por derechos de autor. Algunos derechos reservados.