Shape and spin state model of contact binary (388188) 2006 DP14using combined radar and optical observations

Cannon, Richard E; Rożek, Agata; Brozović, Marina; Pravec, Petr; Snodgrass, Colin; Busch, Michael W; Robinson, James E; Donaldson, Abbie; Holc, Tanja; Benner, Lance A M; Naidu, Shantanu; Kušnirák, Peter; Gardener, Daniel; Kučáková, Hana; Khalouei, Elahe; Pollock, Joseph; Bonavita, Mariangela; Fatka, Petr; Hornoch, Kamil; Sajadian, Sedighe; Alegre, Lara; Amadio, Flavia; Andersen, Michael I; Bozza, Valerio; Burgdorf, Martin J; Columba, Gabriele; Dominik, Martin; Jaimes, R Figuera; Hinse, Tobias C; Hundertmark, Markus; Jørgensen, Uffe G; Longa-Peña, Penelope; Peixinho, Nuno; Rabus, Markus; Rahvar, Sohrab; Rota, Paolo; Skottfelt, Jesper; Southworth, John; Tregloan-Reed, Jeremy

Abstract

Contact binaries are found throughout the solar system. The recent discovery of Selam, the satellite of MBA (152830) Dinkinesh, by the NASA LUCY mission has made it clear that the term ‘contact binary’ covers a variety of different types of bi-modal mass distributions and formation mechanisms. Only by modelling more contact binaries can this population be properly understood. We determined a spin state and shape model for the Apollo group contact binary asteroid (388188) 2006 DP14using ground-based optical and radar observations collected between 2014 and 2023. Radar delay-Doppler images and continuous wave spectra were collected over two days in February 2014, while 16 lightcurves in the Cousins R and SDSS-r filters were collected in 2014, 2022 and 2023. We modelled the spin state using convex inversion before using the SHAPE modelling software to include the radar observations in modelling concavities and the distinctive neck structure connecting the two lobes. We find a spin state with a period of (5.7860 ± 0.0001) hours and pole solution of λ = (180 ± 121)○ and β = ( − 80 ± 7)○ with morphology indicating a 520 m long bi-lobed shape. The model’s asymmetrical bi-modal mass distribution resembles other small NEA contact binaries such as (85990) 1999 JV6or (8567) 1996 HW1, which also feature a smaller ‘head’ attached to a larger ‘body’. The final model features a crater on the larger lobe, similar to several other modelled contact binaries. The model’s resolution is 25 m, comparable to that of the radar images used.

Citation

Cannon, R. E., Rożek, A., Brozović, M., Pravec, P., Snodgrass, C., Busch, M. W., Robinson, J. E., Donaldson, A., Holc, T., Benner, L. A. M., Naidu, S., Kušnirák, P., Gardener, D., Kučáková, H., Khalouei, E., Pollock, J., Bonavita, M., Fatka, P., Hornoch, K., Sajadian, S., …Tregloan-Reed, J. (in press). Shape and spin state model of contact binary (388188) 2006 DP14using combined radar and optical observations. Monthly Notices of the Royal Astronomical Society, 538(4), 1-19. https://doi.org/10.1093/mnras/staf371

• Journal Article Type: Article
• Acceptance Date: Feb 27, 2025
• Online Publication Date: Mar 4, 2025
• Deposit Date: Apr 15, 2025
• Journal: Monthly Notices of the Royal Astronomical Society
• Print ISSN: 0035-8711
• Electronic ISSN: 1365-2966
• Publisher: Oxford University Press
• Peer Reviewed: Peer Reviewed
• Volume: 538
• Issue: 4
• Pages: 1-19
• DOI: https://doi.org/10.1093/mnras/staf371
• Keywords: methods: observational, techniques: photometric, techniques: radar astronomy, minor planets, asteroids: individual: (388188) 2006 DP14
• Public URL: https://keele-repository.worktribe.com/output/1107168
• Publisher URL: https://academic.oup.com/mnras/article/538/4/2311/8052012