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Artículo

Differences between the Pallas collisional family and similarly sized B-type asteroids ?

Alí Lagoa, V.; Licandro, J.; Gil Hutton, Ricardo AlfredoIcon ; Cañada Assandri, Marcela InésIcon ; Delbon, Marisa Ester; De León, J.; Campins, H.; Pinilla Alonso, N.; Kelley, M. S. P.; Hanus, J.
Fecha de publicación: 07/2016
Editorial: EDP Sciences
Revista: Astronomy and Astrophysics
ISSN: 0004-6361
Idioma: Inglés
Tipo de recurso: Artículo publicado
Clasificación temática:
Astronomía

Resumen

Context. B-type asteroids constitute a peculiar spectral class within the C-complex. Previous work has pointed out the difference between the visible geometric albedos of B-types and those of the Pallas collisional family (PCF), whose few members with observed spectra are B-types (one exception out of eight objects). This has been interpreted as being due to compositional differences. However, the PCF members are typically smaller than the spectroscopically classified B-types, and the following possibilities have not been ruled out: the albedo differences might be related to a size-albedo dependence and/or to the generally larger errors of the WISE data and best-fitting values of the derived parameters expected for smaller objects. Aims. We compare albedos and beaming parameters of PCF members and B-types of similar sizes and re-examine our conclusion on the different composition of the PCF. Methods. By modelling their WISE/NEOWISE data, we derived sizes and albedos of all objects whose Sloan Digital Sky Survey reflectances are similar to the typical B-type reflectance spectra. In particular, we derived the so-called infrared beaming parameters (η), effective diameters (D), and corresponding visible geometric albedos (pV), and studied their value distributions. Results. We obtained the effective diameter and geometric visible albedo for ~600 B-type asteroids whose sizes range between 2 and 100 km, approximately half of which have fitted η-values that are inversely correlated to size. We found that the albedo distributions of the PCF is significantly different from that of other B-types in the same size range (2-20 km), and we rule out any size-albedo dependency or biases related to the lower quality of the pV-values of smaller objects. In addition, we also found differences between the η-value distribution of the PCF and the other similarly-sized B-types. Conclusions. The differences in the visible albedos of PCF members and the other B-types of similar sizes is a strong indication that their compositions are different. The trend between beaming parameter and size of the B-types (excluding the PCF) is consistent with the expectation that the surfaces of smaller asteroids have coarser rocks than do those of larger objects (D> 40 km), which are thought to be covered by a finer, more insulating layer of dust.
Palabras clave: Infrared: Planetary Systems , Minor Planets, Asteroids: General , Surveys
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info:eu-repo/semantics/openAccess Excepto donde se diga explícitamente, este item se publica bajo la siguiente descripción: Creative Commons Attribution-NonCommercial-ShareAlike 2.5 Unported (CC BY-NC-SA 2.5)
Identificadores
URI: http://hdl.handle.net/11336/63614
DOI: https://dx.doi.org/10.1051/0004-6361/201527660
URL: https://www.aanda.org/articles/aa/abs/2016/07/aa27660-15/aa27660-15.html
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Articulos(CASLEO)
Articulos de COMPLEJO ASTRONOMICO "EL LEONCITO"
Citación
Alí Lagoa, V.; Licandro, J.; Gil Hutton, Ricardo Alfredo; Cañada Assandri, Marcela Inés; Delbon, Marisa Ester; et al.; Differences between the Pallas collisional family and similarly sized B-type asteroids ?; EDP Sciences; Astronomy and Astrophysics; 591; A14; 7-2016; 1-11
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