THE DUST TAIL OF ASTEROID (3200) PHAETHON

@article{Jewitt2013THEDT,
  title={THE DUST TAIL OF ASTEROID (3200) PHAETHON},
  author={David C. Jewitt and Jing Li and Jessica Agarwal},
  journal={The Astrophysical Journal Letters},
  year={2013},
  volume={771}
}
We report the discovery of a comet-like tail on asteroid (3200) Phaethon when imaged at optical wavelengths near perihelion. In both 2009 and 2012, the tail appears ≳350″ (2.5 × 108 m) in length and extends approximately in the projected anti-solar direction. We interpret the tail as being caused by dust particles accelerated by solar radiation pressure. The sudden appearance and the morphology of the tail indicate that the dust particles are small, with an effective radius ∼1 μm and a combined… 
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The asteroid (3200) Phaethon is widely recognized as the parent of the Geminid meteoroid stream. However, it has never shown evidence for ongoing mass loss or for any form of comet-like activity that
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We present a study of planet-crossing asteroid (3200) Phaethon at three successive perihelia in 2009, 2010, and 2012, using the NASA STEREO spacecraft. Phaethon is clearly detected in 2009 and 2012,
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Some asteroids eject dust, unexpectedly producing transient, comet-like comae and tails. First ascribed to the sublimation of near-surface water ice, mass-losing asteroids (also called “main-belt
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Apollo-type near-Earth asteroid 3200 Phaethon, having a small perihelion distance of q � 0.14 AU, is classified as F- or B-type, one of subclasses among the C-complex (C-, G-, B-, and F-types)
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The thermal evolution of the Geminid meteor stream and the Phaethon–Geminid stream Complex (PGC) are summarized. Sodium contents of Geminid meteor streams are altered thermally, perhaps during
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We present deep optical imaging of Geminid meteor stream parent 3200 Phaethon taken in search of low-level cometary activity (i.e., coma or dust trail). Although no unambiguous cometary behavior was
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Abstract There is evidence that 2201 Oljato and 3200 Phaethon may be inactive cometary remnants. Comet P/Wilson-Harrington (1949 III) was discovered to be the same object as asteroid 4015 1979 VA.
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The history of associating meteor showers with asteroidal-looking objects is long, dating to before the 1983 discovery that 3200 Phaethon moves among the Geminids. Only since the more recent
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The Geminid meteoroid stream formation and evolution were studied by the method of nested polynomials. The stream has two layers formed due to differences in orbital parameters of particles ejected
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