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    Shape model and spin-state analysis of PHA contact binary (85990) 1999 JV6 from combined radar and optical observations

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    Author
    Rożek, A.
    Lowry, S. C.
    Nolan, M. C.
    Taylor, P. A.
    Benner, L. A. M.
    Fitzsimmons, A.
    Zegmott, T. J.
    Weissman, P. R.
    Green, S. F.
    Rozitis, B.
    Snodgrass, C.
    Smythe, W. D.
    Hicks, M. D.
    Howell, E. S.
    Virkki, A. K.
    Aponte-Hernandez, B.
    Rivera-Valentín, E. G.
    Rodriguez-Ford, L. A.
    Zambrano-Marin, L. F.
    Brozović, M.
    Naidu, S. P.
    Giorgini, J. D.
    Snedeker, L. G.
    Jao, J. S.
    Ghigo, F. D.
    Show allShow less
    Affiliation
    Univ Arizona, Lunar & Planetary Lab
    Issue Date
    2019-11-13
    Keywords
    minor planets
    asteroids: individual: (85990) 1999 JV6
    methods: observational
    methods: data analysis
    techniques: photometric
    techniques: radar astronomy
    radiation mechanisms: thermal
    
    Metadata
    Show full item record
    Publisher
    EDP SCIENCES S A
    Citation
    Rożek, A., Lowry, S. C., Nolan, M. C., Taylor, P. A., Benner, L. A. M., Fitzsimmons, A., … Ghigo, F. D. (2019). Shape model and spin-state analysis of PHA contact binary (85990) 1999 JV6 from combined radar and optical observations. Astronomy & Astrophysics, 631, A149. https://doi.org/10.1051/0004-6361/201936302 ‌
    Journal
    ASTRONOMY & ASTROPHYSICS
    Rights
    Copyright © ESO 2019.
    Collection Information
    This item from the UA Faculty Publications collection is made available by the University of Arizona with support from the University of Arizona Libraries. If you have questions, please contact us at repository@u.library.arizona.edu.
    Abstract
    Context. The potentially hazardous asteroid (85990) 1999 JV6 has been a target of previously published thermal-infrared observations and optical photometry. It has been identified as a promising candidate for possible Yarkovsky-O'Keefe-Radzievskii-Paddack (YORP) effect detection. Aims. The YORP effect is a small thermal-radiation torque considered to be a key factor in spin-state evolution of small Solar System bodies. In order to detect YORP on 1999 JV6 we developed a detailed shape model and analysed the spin-state using both optical and radar observations. Methods. For 1999 JV6, we collected optical photometry between 2007 and 2016. Additionally, we obtained radar echo-power spectra and imaging observations with Arecibo and Goldstone planetary radar facilities in 2015, 2016, and 2017. We combined our data with published optical photometry to develop a robust physical model. Results. We determine that the rotation pole resides at negative latitudes in an area with a 5 degrees radius close to the south ecliptic pole. The refined sidereal rotation period is 6.536787 +/- 0.000007 h. The radar images are best reproduced with a bilobed shape model. Both lobes of 1999 JV6 can be represented as oblate ellipsoids with a smaller, more spherical component resting at the end of a larger, more elongated component. While contact binaries appear to be abundant in the near-Earth population, there are only a few published shape models for asteroids in this particular configuration. By combining the radar-derived shape model with optical light curves we determine a constant-period solution that fits all available data well. Using light-curve data alone we determine an upper limit for YORP of 8.5 x 10(-8) rad day(-2). Conclusions. The bifurcated shape of 1999 JV6 might be a result of two ellipsoidal components gently merging with each other, or a deformation of a rubble pile with a weak-tensile-strength core due to spin-up. The physical model of 1999 JV6 presented here will enable future studies of contact binary asteroid formation and evolution.
    ISSN
    0004-6361
    DOI
    10.1051/0004-6361/201936302
    Version
    Final published version
    ae974a485f413a2113503eed53cd6c53
    10.1051/0004-6361/201936302
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    UA Faculty Publications

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