Astronomy:3200 Phaethon

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3200 Phaethon
Radar image of 3200 Phaethon taken by Arecibo, December 17, 2017
Discovery
Discovered by
Discovery dateOctober 11, 1983
Designations
(3200) Phaethon
Pronunciation/ˈfeɪ.əθɒn/
Named afterPhaëthon
1983 TB
Minor planet category
AdjectivesPhaethonian /feɪəˈθoʊniən/[2]
Orbital characteristics[1]
Epoch April 27, 2019 (JD 2458000.5)
Uncertainty parameter 0
Observation arc12,941 days (35.43 yr)
|{{{apsis}}}|helion}}2.4028 astronomical unit|AU (359 million km)
|{{{apsis}}}|helion}}0.13998 AU (20.9 million km)
1.2714 AU (190 million km)
Eccentricity0.88990
Orbital period523.6 days (1.434 yr)
Average Orbital speed19.9 km/s (45,000 mph)
Mean anomaly313.94°
Mean motion0° 41m 15.108s / day
Inclination22.260°
Longitude of ascending node265.22°
|{{{apsis}}}|helion}}May 15, 2022[3]
322.19°
Earth MOID0.01955 AU (2.92 million km)
Venus MOID 0.0469 AU (7.02 million km)[4]
Jupiter MOID2.7375 AU (410 million km)
TJupiter4.510
Physical characteristics
Dimensions6.13±0.05 × 4.40±0.06 km[5]
Mean diameter5.8 km (3.6 mi)[6]
Rotation period3.604 hours (0.1502 d)[1]
Geometric albedo0.1066±0.011[1]
F-type asteroid[1][7]
Apparent magnitude10.7 (December 14, 2017)
Absolute magnitude (H)14.6[1]


3200 Phaethon (/ˈfeɪ.əˌθɒn/; previously sometimes spelled Phæton), provisionally designated 1983 TB, is an active[8] Apollo asteroid with an orbit that brings it closer to the Sun than any other named asteroid (though there are numerous unnamed asteroids with smaller perihelia, such as (137924) 2000 BD19).[9] For this reason, it was named after the Greek Hero, Phaëthon, son of the sun god Helios. It is 5.8 km (3.6 mi) in diameter[6] and is the parent body of the Geminids meteor shower of mid-December. With an observation arc of 35+ years, it has a very well determined orbit.[1] The 2017 Earth approach distance of about 10 million km was known with an accuracy of ±700 m.[1]

Discovery

Phaethon was the first asteroid to be discovered using images from a spacecraft. Simon F. Green and John K. Davies discovered it in images from October 11, 1983, while searching Infrared Astronomical Satellite (IRAS) data for moving objects. It was formally announced on October 14 in IAUC 3878 along with optical confirmation by Charles T. Kowal, who reported it to be asteroidal in appearance. Its provisional designation was 1983 TB, and it later received the numerical designation and name 3200 Phaethon in 1985.

Orbital characteristics

Animation of 3200 Phaethon's orbit
   Sun ·    Mercury ·    Venus ·    Earth ·    Mars ·   3200 Phaethon

Phaethon is categorized as an Apollo asteroid, as its orbital semi-major axis is greater than that of the Earth's at 1.27 astronomical unit|AU (190 million km; 118 million mi). It is also suspected to be a member of the Pallas family of asteroids.[10]

Its most remarkable distinction is that it approaches the Sun closer than any other named asteroid: its perihelion is only 0.14 AU (20.9 million km; 13.0 million mi) — less than half of Mercury's perihelial distance. It is a Mercury-, Venus-, Earth-, and Mars-crosser as a result of its high orbital eccentricity. The surface temperature at perihelion could reach around 1,025 K (750 °C; 1,390 °F).

Phaethon is a possible candidate for detecting general relativistic and/or solar oblateness effects in its orbital motion due to the frequent close approaches to the Sun.[11] The Apollo asteroids (155140) 2005 UD and (225416) 1999 YC share similar orbits with Phaethon, suggesting a possible common breakup origin.[12][13]

Potentially hazardous asteroid

Phaethon is categorized as a potentially hazardous asteroid (PHA),[1][14] but that does not mean there is a near-term threat of an impact. It is a potentially hazardous asteroid merely as a result of its size (absolute magnitude H ≤ 22) and Earth minimum orbit intersection distance (Earth MOID ≤ 0.05 AU).[15] The Earth minimum orbit intersection distance (E-MOID) is 0.01945 AU (2,910,000 km; 1,808,000 mi), which is defined by the shortest distance between the orbit of Phaethon and the orbit of Earth.[1] With a 30+ year observation arc, the orbit of Phaethon is very well understood with very small uncertainties.[1] Close approaches of Phaethon are well constrained for the next 400 years.[11]

Template:Large near earth asteroid flybys 10LD

Physical characteristics

"Rock comet" redirects here. For other rocky bodies exhibiting comet-like activity, see active asteroid.
Phaethon's dust ejection is likely caused by a mechanism similar to how mud in a dry lake bottom cracks from heat

Phaethon is an asteroid with fairly unusual characteristics in that its orbit more closely resembles that of a comet than an asteroid; it has been referred to as a "rock comet".[16] In studies performed by NASA's STEREO spacecraft in 2009 and 2012, rapid brightening and a visible tail have been observed.[17][18][19] It is possible that the Sun's heat is causing fractures similar to mudcracks in a dry lake bed.[20] This occurs because Phaethon's orbit takes it closer to the Sun than any other named asteroid (0.14 AU at perihelion) causing extreme heating and enough solar radiation pressure to push any separated pieces off the asteroid's surface. Since its discovery, several other objects were found exhibiting mixed cometary and asteroidal features, such as 133P/Elst–Pizarro, leading to a new class of objects dubbed "active asteroids".[8]

In 2007, observations revealed that Phaethon was blue in color [21] corresponding to a B-type asteroid in the Bus taxonomy. In 2020, polarimetric study revealed Phaethon has a surface with steep slopes covered by a mix of regolith with larger pebbles.[22] Phaethon's composition fits both, the notion of its cometary origin and that of an active asteroid; it is classified as a F-type asteroid because it is composed of dark material[1][7] or a B-type asteroid because of its blue color.[23] In 2009,[21] showed that the spectral shape is similar to that of aqueously altered CI/CM meteorites. Later, in 2022, it was shown [24][25] how Phaethon's blue color and its rock-comet-like emission activity could be explained by the effects of the intense solar heating at perihelion causing sublimation of any darkish-red refractory organic, nano-phase iron (nFe0), and pyroxene materials on its surface.

Analysis of a mid-infrared spectral emissivity spectrum from the Spitzer Space Telescope showed Phaethon to be linked to the rare Yamato-type (CY) carbonaceous chondrites.[26] This link rules out other carbonaceous meteorite types, although the understanding of the origins of CYs are evolving.[27] Further analysis of this spectrum confirmed the presence of Mg-rich olivine, carbonates, and Fe-sulfides. Until further studies were done in 2023, it was believed that thermal decomposition and outgassing of these minerals during perihelion led to dust ejection, possibly explaining a faint observed tail and the formation of the Geminid meteor stream. However in a 2023 NASA study[28] imaging from the SOHO spacecraft revealed that the material emitted from the asteroid was sodium gas, with filtered images revealing no sign of dust at all. This cast doubt on the origin of the Geminids being dust and material cast off from Phaethon during periodic solar perihelions, and instead invited speculation of an ancient breakup event.

Meteor shower

Shortly after its discovery, Fred Whipple noted that Phaethon's orbital elements were extremely similar to those of the Geminid meteor shower,[29] indicating that Phaethon was the meteor shower's long-sought parent body.

Planned flyby

DESTINY+ spacecraft have a planned flyby over asteroid 3200 Phaethon.

DESTINY+ (Demonstration and Experiment of Space Technology for INterplanetary voYage Phaethon fLyby dUSt science) is a planned mission to fly by 3200 Phaethon, as well as various minor bodies originating from it. The spacecraft is being developed by the Japanese space agency JAXA and will demonstrate advanced technologies for future deep space exploration. DESTINY+ is planned to be launched no earlier than 2028.[30]

Close approaches

Phaethon approached to 0.120895 astronomical unit|AU (18,085,600 km; 11,237,900 mi) of Earth on December 10, 2007,[1] and was detected by radar at Arecibo.[11] When Phaethon came to perihelion in July 2009, it was found to be brighter than expected.[31][32] During its approach, the STEREO-A spacecraft detected an unexpected brightening, roughly by a factor of two.[16]

2010 approach

Phaethon imaged on December 25, 2010, with the 37-cm f/14 Rigel telescope at Winer Observatory by Marco Langbroek

2017 approach

On December 16, 2017, at 23:00 UT, Phaethon passed 0.06893169 AU (10,312,034 km; 6,407,601 mi) from Earth (27 lunar distances).[1] The Earth approach distance was known with a 3-sigma precision of ±700 m.[1][lower-alpha 1] This was the best opportunity to date for radar observations by Goldstone and Arecibo, with a resolution of 75 meters/pixel (246 feet/pixel).[11]

The asteroid was bright enough to see in small telescopes, peaking at magnitude 10.8 between December 13–15 while dimming slightly to magnitude 11 on December 16 at closest approach.[33] Arecibo made observations of Phaethon from December 15–19.[6] It will not make an Earth approach closer than the 2017 passage until December 14, 2093, when it will pass 0.01981 AU (2,964,000 km; 1,841,000 mi) from Earth.[1][34]

Path of 3200 Phaethon in the sky during December 2017
Time lapse taken through a telescope in Riga, Latvia (December 10, 2017)
Phaethon at maximum angular velocity, December 15, 2017, 18:47:13–19:24:50 UTC

Notes

  1. ↑ In 2014, JPL 374 (solution date 2014-Sep-12) showed a 2017 Earth approach distance with a precision of ±80 km. Math: (MAX−MIN) * AU / 2

References

  1. ↑ 1.00 1.01 1.02 1.03 1.04 1.05 1.06 1.07 1.08 1.09 1.10 1.11 1.12 1.13 1.14 1.15 "JPL Small-Body Database: 3200 Phaethon (1983 TB)". JPL Small-Body Database. Jet Propulsion Laboratory. https://ssd.jpl.nasa.gov/tools/sbdb_lookup.html#/?sstr=3200&view=OPDCRA. 
  2. ↑ phaeton (3rd ed.), Oxford University Press, September 2005, http://oed.com/search?searchType=dictionary&q=phaeton  (Subscription or UK public library membership required.)
  3. ↑ JPL Horizons Observer Location: @sun (Perihelion occurs when deldot changes from negative to positive.)
  4. ↑ "(3200) Phaethon Orbit". Minor Planet Center. https://minorplanetcenter.net/db_search/show_object?object_id=3200. 
  5. ↑ "(3200) Phaethon 2021 Oct 3". Hayamizu Astro Laboratory. 3 October 2021. http://www.hal-astro-lab.com/data/occult-e/2021Oct3_Phaethon_DAMIT.png. Retrieved 14 February 2022. 
  6. ↑ 6.0 6.1 6.2 Agle, D. C.; Brown, Dwayne; Farukhi, Suraiya (December 22, 2017). "Arecibo Radar Returns with Asteroid Phaethon Images". NASA. https://www.jpl.nasa.gov/news/news.php?feature=7030. 
  7. ↑ 7.0 7.1 Kartashova, A.; Husarik, M.; Ivanova, O.; Kokhirova, G.; Bakanas, E.; Sokolov, I.; Khamroev, U. Kh.; Ibragimov, A. A. (June 5, 2019), "Photometric observations of the asteroid 3200 Phaethon using small and middle telescopes", Contributions of the Astronomical Observatory Skalnate Pleso 49 (2): 367, Bibcode: 2019CoSka..49..367K 
  8. ↑ 8.0 8.1 Jewitt, David; Hsieh, Henry; Agarwal, Jessica (2015). "The Active Asteroids". in Michel, P.; others. Asteroids IV. University of Arizona. pp. 221–241. doi:10.2458/azu_uapress_9780816532131-ch012. ISBN 9780816532131. Bibcode: 2015aste.book..221J. http://www2.ess.ucla.edu/~jewitt/papers/2015/JHA15.pdf. Retrieved 2020-01-30. 
  9. ↑ "JPL Small-Body Database Search Engine — Constraints: asteroids and q < 0.141 (au)". Jet Propulsion Laboratory. http://ssd.jpl.nasa.gov/sbdb_query.cgi?obj_group=all;obj_kind=ast;obj_numbered=all;OBJ_field=0;ORB_field=0;c1_group=ORB;c1_item=Bi;c1_op=%3C;c1_value=0.141;table_format=HTML;max_rows=100;format_option=comp;c_fields=AcBhBgBjBiBnBsCkCqAi;.cgifields=format_option;.cgifields=obj_kind;.cgifields=obj_group;.cgifields=obj_numbered;.cgifields=ast_orbit_class;.cgifields=table_format;.cgifields=com_orbit_class&query=1&c_sort=BiA.  Take notice of the orbit condition number (the lower the number, the lower the orbit's uncertainty).
  10. ↑ Jaggard, Victoria (October 12, 2010). "Exploding Clays Drive Geminids Sky Show?". National Geographic. https://voices.nationalgeographic.org/2010/10/12/geminids_meteor_shower_driven_by_exploding_clays/. 
  11. ↑ 11.0 11.1 11.2 11.3 Benner, Lance A. M. (2017). "Goldstone Radar Observations Planning: Asteroid 3200 Phaethon". NASA/JPL Asteroid Radar Research. https://echo.jpl.nasa.gov/asteroids/Phaethon/Phaethon_planning.2017.html. 
  12. ↑ Devogèle, MaximeExpression error: Unrecognized word "etal". (June 2020). "New Evidence for a Physical Link between Asteroids (155140) 2005 UD and (3200) Phaethon". The Planetary Science Journal 1 (1): 15. doi:10.3847/PSJ/ab8e45. 15. Bibcode: 2020PSJ.....1...15D. 
  13. ↑ Cukier, W. Z.; Szalay, J. R. (June 1, 2023). "Formation, Structure, and Detectability of the Geminids Meteoroid Stream". The Planetary Science Journal 4 (6): 109. doi:10.3847/psj/acd538. ISSN 2632-3338. Bibcode: 2023PSJ.....4..109C. 
  14. ↑ Phillips, Tony (December 3, 2007). "Asteroid Shower". NASA. https://science.nasa.gov/science-news/science-at-nasa/2007/03dec_asteroidshower. 
  15. ↑ "NEO Groups". NASA. https://cneos.jpl.nasa.gov/about/neo_groups.html. 
  16. ↑ 16.0 16.1 Jewitt, David; Li, Jing (2010). "Activity in Geminid Parent (3200) Phaethon". The Astronomical Journal 140 (5): 1519. doi:10.1088/0004-6256/140/5/1519. Bibcode: 2010AJ....140.1519J. 
  17. ↑ Jewitt, David; Li, Jing; Agarwal, Jessica (2013). "The Dust Tail of Asteroid (3200) Phaethon". The Astrophysical Journal Letters 771 (2): L36. doi:10.1088/2041-8205/771/2/L36. Bibcode: 2013ApJ...771L..36J. 
  18. ↑ Li, Jing; Jewitt, David (2013). "Recurrent Perihelion Activity in (3200) Phaethon". Astronomical Journal 145 (6): 154. doi:10.1088/0004-6256/145/6/154. Bibcode: 2013AJ....145..154L. https://iopscience.iop.org/article/10.1088/0004-6256/145/6/154. Retrieved 2022-01-22. 
  19. ↑ Jewitt, David; Li, Jing (2010). "Activity in Geminid Parent (3200) Phaethon". Astronomical Journal 140 (5): 1519–1527. doi:10.1088/0004-6256/140/5/1519. Bibcode: 2010AJ....140.1519J. https://iopscience.iop.org/article/10.1088/0004-6256/140/5/1519. Retrieved 2022-01-22. 
  20. ↑ Sutherland, Paul (September 10, 2013). "Why an asteroid is crumbling into meteor dust". Skymania.com. http://www.skymania.com/wp/2013/09/why-an-asteroid-is-crumbling-into-meteor-dust.html/. 
  21. ↑ 21.0 21.1 Licandro, J.; Campins, H.; Mothé-Diniz, T.; Pinilla-Alonso, N.; de León, J. (2007). "The nature of comet-asteroid transition object (3200) Phaethon". Astronomy & Astrophysics 461 (2): 751–757. doi:10.1051/0004-6361:20065833. Bibcode: 2007A&A...461..751L. https://ui.adsabs.harvard.edu/abs/2007A&A...461..751L. Retrieved 2026-02-28. 
  22. ↑ Golubeva, L. F.; Shestopalov, D. I.; Kvaratskhelia, O. I. (2020). "Polarimetric properties of asteroid 3200 Phaethon". arXiv:2001.00789 [astro-ph.EP].
  23. ↑ Clark, Beth; Ziffer, Julie; Nesvorny, David (2010). "Spectroscopy of B-type asteroids: Subgroups and meteorite analogs". Journal of Geophysical Research 115 (E6): E06005. doi:10.1029/2009JE003478. Bibcode: 2010JGRE..115.6005C. https://stars.library.ucf.edu/facultybib2010/48. 
  24. ↑ Lisse, Carey; Steckloff, Jordan (2022). "Thermal alteration and differential sublimation can create Phaethon's "rock comet" activity and blue color". Icarus 381. doi:10.1016/j.icarus.2022.114995. Bibcode: 2022Icar..38114995L. 
  25. ↑ How the bluest asteroid in the solar system got its color Tereza Pultarova, Space.com. June 16th, 2022
  26. ↑ MacLennan, Eric; Granvik, Mikael (2 November 2023). "Thermal decomposition as the activity driver of near-Earth asteroid (3200) Phaethon". Nature Astronomy 8: 60–68. doi:10.1038/s41550-023-02091-w. 
  27. ↑ Schrader, D. L.; Torrano, Z. A.; Foustoukos, D. I.; Alexander, C. M. O’D.; Render, J.; Brennecka, G. A. (Feb 2025). "Reassessing the proposed "CY chondrites": Evidence for multiple meteorite types and parent bodies from Cr-Ti-H-C-N isotopes and bulk elemental compositions". Geochim. Cosmochim. Acta 390: 24–37. doi:10.1016/j.gca.2024.12.021. Bibcode: 2025GeCoA.390...24S. 
  28. ↑ Zhang, Qicheng; Battams, Karl (25 April 2023). "Sodium Brightening of (3200) Phaethon near Perihelion". The Planetary Science Journal 4: 70-71. doi:10.3847/PSJ/acc866. 
  29. ↑ Whipple, F. L. (October 25, 1983). Marsden, B. G.. ed. "1983 TB and the Geminid Meteors". IAU Circular (3881): 1. Bibcode: 1983IAUC.3881....1W. 
  30. ↑ "宇宙科学・探査ミッションの進捗状況について" (in ja). ISAS. CAO. 9 October 2024. p. 11. https://www8.cao.go.jp/space/comittee/27-kagaku/kagaku-dai63/siryou2.pdf. 
  31. ↑ Shanklin, Jonathan (2009). "Comet Section: 2009 News". British Astronomical Association. http://www.ast.cam.ac.uk/~jds/news09.htm. 
  32. ↑ Battams, K.; Watson, A. (June 2009). "(3200) Phaethon". IAU Circular (9054): 3. Bibcode: 2009IAUC.9054....3B. 
  33. ↑ "(3200) Phaethon: Ephemerides for December 2017". NEODyS-2. University of Pisa Department of Mathematics. https://newton.spacedys.com/neodys/index.php?pc=1.1.3.1&n=3200&oc=500&y0=2017&m0=12&d0=01&h0=0&mi0=0&y1=2017&m1=12&d1=31&h1=0&mi1=0&ti=1.0&tiu=days. 
  34. ↑ "(3200) Phaethon: Close Approaches". NEODyS-2. University of Pisa Department of Mathematics. https://newton.spacedys.com/neodys/index.php?pc=1.1.8&n=3200. 



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