Volume 631, November 2019
|Number of page(s)||28|
|Section||Planets and planetary systems|
|Published online||13 November 2019|
Shape model and spin-state analysis of PHA contact binary (85990) 1999 JV6 from combined radar and optical observations★,★★
Centre for Astrophysics and Planetary Science, University of Kent,
2 Lunar and Planetary Laboratory, University of Arizona, Tucson, Arizona, USA
3 Lunar and Planetary Institute, Universities Space Research Association, Houston, Texas, USA
4 Planetary Science Section, Jet Propulsion Laboratory/Caltech, Pasadena, California, USA
5 Astrophysics Research Centre, Queens University Belfast, Belfast, UK
6 Planetary Sciences Institute, Tucson, Arizona, USA
7 Planetary and Space Sciences, School of Physical Sciences, The Open University, Milton Keynes, UK
8 Institute for Astronomy, University of Edinburgh, Royal Observatory, Edinburgh, UK
9 Arecibo Observatory, University of Central Florida, Arecibo, Porto Rico, USA
10 National Radio Astronomy Observatory, Green Bank, West Virginia, USA
Accepted: 1 October 2019
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° 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 × 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.
Key words: minor planets, asteroids: individual: (85990) 1999 JV6 / methods: observational / methods: data analysis / techniques: photometric / techniques: radar astronomy / radiation mechanisms: thermal
Table A.2 is only available at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (184.108.40.206) or via http://cdsarc.u-strasbg.fr/viz-bin/cat/J/A+A/631/A149
© ESO 2019
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