A new non-convex model of the binary asteroid (809) Lundia obtained with the SAGE modelling technique

Bibcode
2017MNRAS.471..941B
DOI
10.1093/mnras/stx1603
Bartczak, P.; Kryszczyńska, A.; Dudziński, G.; Polińska, M.; Colas, F.; Vachier, F.; Marciniak, A.; Pollock, J.; Apostolovska, G.; Santana-Ros, T.; Hirsch, R.; Dimitrow, W.; Murawiecka, M.; Wietrzycka, P.; Nadolny, J.
Bibliographical reference

Monthly Notices of the Royal Astronomical Society, Volume 471, Issue 1, p.941-947

Advertised on:
10
2017
Journal
Monthly Notices of the Royal Astronomical Society
Number of authors
15
IAC number of authors
1
Citations
4
Refereed citations
2
Description
We present a new non-convex model of the binary asteroid (809) Lundia. A SAGE (Shaping Asteroids with Genetic Evolution) method using disc-integrated photometry only was used for deriving physical parameters of this binary system. The model of (809) Lundia improves former system's pole solution and gives the ecliptic coordinates of the orbit pole - λ = 122°, β = 22°, σ = ±5° - and the orbital period of 15.415 74 ± 0.000 01 h. For scaling our results, we used an effective diameter (Deff) of 9.6 ± 1.1 km obtained from Spitzer observations. The non-convex shape description of the components permitted a refined calculation of the components' volumes, leading to a density estimation of 2.5 ± 0.2 g cm-3 and a macroporosity of 13-23 per cent. The intermediate-scale features of the model may also offer new clues on the components' origin and evolution.
Type
Refereed
Methods
Techniques

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