J/A+A/672/A48 Compositions of binary asteroids (Minker+, 2023)
Deficit of primitive compositions in binary asteroids and pairs.
Minker K., Carry B.
<Astron. Astrophys. 672, A48 (2023)>
=2023A&A...672A..48M 2023A&A...672A..48M (SIMBAD/NED BibCode)
ADC_Keywords: Solar system ; Minor planets ; Binaries, orbits
Keywords: minor planets - asteroids: general - methods: statistical
Abstract:
Small binary asteroid systems and pairs are thought to form through
fission induced by spin up via the
Yarkovsky-O'Keefe-Radzievskii-Paddack (YORP) effect. This process is
expected to depend on their structural strength, hence composition.
We aim to determine how taxonomic classes, used as a proxy for
composition, distribute amongst binary asteroids and asteroid pairs
compared to the general population.
We compare the distribution of taxonomic classes of binary systems and
pairs with that of a reference sample of asteroids. We build this
sample by selecting asteroids to reproduce the orbital and size
distribution of the binaries and pairs to minimize potential biases
between samples.
A strong deficit of primitive compositions (C, B, P, D types) among
binary asteroids and asteroid pairs is identified, as well as a strong
excess of asteroids with mafic-silicate rich surface compositions (S,
Q, V, A types). Conclusions. Amongst low mass, rapidly rotating
asteroids, those with mafic-silicate rich compositions are more likely
to form multiple asteroid systems than their primitive counterparts.
Description:
Details of asteroids considered in the study are provided, as an
extension of tables A.1 to A.8.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
tablea.dat 162 10968 Details of asteroids considered in the study
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Byte-by-byte Description of file: tablea.dat
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Bytes Format Units Label Explanations
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1- 13 A13 --- Set Set which asteroid belongs to (1)
15- 22 F8.1 --- Num Asteroid number
24- 39 A16 --- Name Asteroid name
41- 48 F8.6 --- a Semi-major axis
50- 57 F8.6 --- e Orbital eccentricity
59- 67 F9.6 --- i Orbital inclination
69- 74 F6.3 km Diam ? Primary diameter
76- 81 F6.4 km e_Diam ? Uncertainty in diameter
83-101 A19 --- r_Diam Citation for diameter (BibCodbe)
103-108 F6.4 --- pV ? Albedo
110-116 F7.5 --- e_pV ? Uncertainty in albedo
118-121 A4 --- TaxMethod Method used to determine taxonomy (2)
123-131 A9 --- TaxScheme Scheme used to determine taxonomy
133-135 A3 --- Class Taxonomic class
137-142 A6 --- Waverange Waverange used to determine taxonomy
144-162 A19 --- TaxRef Citation for taxonomy (BibCodbe)
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Note (1): Set membership as follows:
bin-spec = spectroscopic binaries set (table A.1)
bin-phot = photometric binaries set (table A.2)
pair-phot = photometric pairs set (table A.3)
pair-spec = spectroscopic pairs set (table A.4)
bin-phot-ref = photometric binaries reference set (table A.5)
bin-spec-ref = spectroscopic binaries reference set (table A.6)
pair-phot-ref = photometric pairs reference set (table A.7)
pair-spec-ref = spectroscopic pairs reference set (table A.8)
Note (2): Method used to determine taxonomy as follows:
spec = spectroscopy
phot = photometry
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History:
From Kate Minker, kate.minker(at)oca.eu
Acknowledgements:
We thank CNES for supporting K. Minker in her internship during her
Masters of astrophysics (MAUCA: http://mauca.oca.eu). This research
used the VO TOPCAT software (Taylor, 2005). The properties of Solar
System Object are from the service SsODNet.ssoCard of the Service des
ephemerides de l'IMCCE through its Solar System Portal
(https://ssp.imcce.fr). We thank all the developers and maintainers of
resources for the community.
(End) Patricia Vannier [CDS] 03-Mar-2023