2017/06/23 by P. Bartczak, A. Kryszczyńska, G. Dudziński +14 · 2 citations
Mathematics · Physics and Astronomy · #Aerospace engineering #Asteroid #Astro and Planetary Science #Astronomy #Astrophysics #Binary number #Celestial mechanics #Ecliptic #Geometry #Mathematics #Orbit (dynamics) #Orbital elements #Photometry (optics) #Physics #Planetary Science and Exploration #Regular polygon #Scaling #Stellar, planetary, and galactic studies #astro-ph.EP
paper · pdf · doi:10.1093/mnras/stx1603
published in Monthly Notices of the Royal Astronomical Society 471(1), 941-947 (Oxford University Press)
openalex publication_date 2017/06/23 · arxiv created 2019/05/20 · arxiv updated 2019/05/22 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05
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.