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@ARTICLE{,
    author = {Hanu{\v s}, J. and Vokrouhlick{\'{y}}, D. and Delbo', M. and Farnocchia, D. and Polishook, D. and Pravec, P. and Hornoch, K. and Ku{\v c}{\'{a}}kov{\'{a}}, H. and Ku{\v s}nir{\'{a}}k, P. and Stephens, R. and Warner, B.},
  keywords = {asteroids: individual: (3200) Phaethon, astrometry, Astrophysics - Earth and Planetary Astrophysics, celestial mechanics, methods: numerical, methods: observational, minor planets},
     month = {dec},
     title = {(3200) Phaethon: Bulk density from Yarkovsky drift detection},
   journal = {Astronomy and Astrophysics},
    volume = {620},
      year = {2018},
     pages = {L8},
      issn = {0004-6361},
       url = {https://ui.adsabs.harvard.edu/abs/2018A&A...620L...8H},
  abstract = {Context. The recent close approach of the near-Earth asteroid (3200)},
={Phaethon offered a rare opportunity to obtain high-quality observational, data of various types. <BR /> Aims: We used the newly obtained optical, light curves to improve the spin and shape model of Phaethon and to, determine its surface physical properties derived by thermophysical, modeling. We also used the available astrometric observations of, Phaethon, including those obtained by the Arecibo radar and the Gaia, spacecraft, to constrain the secular drift of the orbital semimajor, axis. This constraint allowed us to estimate the bulk density by, assuming that the drift is dominated by the Yarkovsky effect. <BR />, Methods: We used the convex inversion model to derive the spin, orientation and 3D shape model of Phaethon, and a detailed numerical, approach for an accurate analysis of the Yarkovsky effect. <BR />, Results: We obtained a unique solution for Phaethon's pole orientation, 47 ° ) ecliptic longitude and latitude (both with an, uncertainty of 5°), and confirm the previously reported thermophysical, properties (D = 5.1 ± 0.2 km, Γ = 600 ± 200J m<SUP>-2</SUP>, s<SUP>-0.5</SUP> K<SUP>-1</SUP>). Phaethon has a top-like shape with, possible north-south asymmetry. The characteristic size of the regolith, 2 cm. The orbit analysis reveals a secular drift of the, (6.9 ± 1.9)×10<SUP>-4</SUP> au Myr<SUP>-1</SUP>. With, the derived volume-equivalent size of 5.1 km, the bulk density is 1.67 ±, 5.8 km, as, suggested by radar data, the bulk density would decrease to 1.48 ± 0.42, g cm<SUP>-3</SUP>. We further investigated the suggestion that Phaethon, may be in a cluster with asteroids (155140) 2005 UD and (225416) 1999 YC, that was formed by rotational fission of a critically spinning parent, body. <BR /> Conclusions: Phaethon's bulk density is consistent with, typical values for large (&gt; 100 km) C-complex asteroids and supports, its association with asteroid (2) Pallas, as first suggested by, dynamical modeling. These findings render a cometary origin unlikely for, Phaethon., 10.1051/0004-6361/201834228, eprint: arXiv:1811.10953},
}