289P/Blanpain

289P/Blanpain
Infrared image of 289P/Blanpain taken by NEOWISE on 11 January 2020
Discovery[1][2]
Discovered byJean-Jacques Blanpain
Discovery siteMarseille, France
Discovery date28 November 1819
22 November 2003[3]
Designations
D/1819 W1, P/2003 WY25
1819 IV[4]
Orbital characteristics[5]
Epoch21 November 2025 (JD 2461000.5)
Observation arc204.63 years[a]
Number of
observations		690
Aphelion5.133 AU
Perihelion0.954 AU
Semi-major axis3.044 AU
Eccentricity0.68642
Orbital period5.309 years
Inclination5.900°
68.891°
Argument of
periapsis		9.878°
Mean anomaly40.964°
Last perihelion14 April 2025
Next perihelion6 August 2030[6]
TJupiter2.817
Earth MOID0.017 AU
Jupiter MOID0.217 AU
Physical characteristics[7]
Mean radius
160 m (520 ft)[8]
8.85±0.39 hours[9]
0.04 (assumed)
Comet total
magnitude (M1)		22.0

289P/Blanpain, formerly D/1819 W1 (Blanpain) is a Jupiter-family comet with an orbital period of 5.2 years. It was discovered by Jean-Jacques Blanpain on 28 November 1819, but was considered lost until it was recovered in 2013.[10] It was last observed in 2024.[5]

Observational history

The comet was discovered by Jean-Jacques Blanpain on 28 November 1819. Blanpain described the comet as having a "very small and confused nucleus".[1] Another independent discovery was made on December 5 of that year by Jean-Louis Pons. Following this the comet was lost, and was given the designation 'D' (Disappeared or Dead).

However, in 2003, the orbital elements of newly discovered asteroid 2003 WY25 were calculated by Marco Micheli and others to be a probable match for the lost comet.[11] On 12 December 2003, it approached Earth at a distance of 0.025 AU (3.7 million km; 2.3 million mi).[7] Further observations of the asteroid in 2005 by David C. Jewitt using the University of Hawaii 2.2 m telescope on Mauna Kea, appeared to reveal a faint coma, which supports the theory that 2003 WY25 is the lost comet, or a part of it.[8] The comet was officially established as periodic comet 289P in July 2013, after being rediscovered by the Pan-STARRS survey during an outburst event.[2]

The comet underwent a major outburst in July 2013, when it brightened by 9 magnitudes, one of the largest observed comet outbursts.[12] The comet was first spotted in images obtained by Pan-STARRS on 4 July 2013, having a reported magnitude of about 20, and brightened to a magnitude of about 17.5 and featured a coma about 30 arcseconds across and a broad tail.[2][13] It is estimated that the comet lost about 108 kg of dust, which corresponds to about 1% of the comet's mass. The comet then was located 3.9 AU (580 million km; 360 million mi) from the Sun.[12]

289P was better viewed near and after the December 2019 perihelion passage. On 11 January 2020, the comet approached Earth at a distance of 0.091 AU (13.6 million km; 8.5 million mi). The next close approach will take place on 6 November 2035, at a distance of 0.082 AU (12.3 million km; 7.6 million mi).[7]

Physical characteristics

The observations of the comet by the University of Hawaii 2.2 m telescope indicate the nucleus of the comet is quite small. Assuming an albedo of 0.04, which is the mean value for short period comets, its radius is about 160 m (520 ft), although the presence of coma and unknown phase function means that there is quite some uncertainty. However at that time it was the smallest known cometary nucleus.[8] Observations of the comet in 2019–20 by NEOWISE indicate a rotational period of 8.8536±0.386 hours or 15.6 hours, with the former being more likely.[9]

The ejected dust masses are 4100±200 kg inbound and 1700±200 kg outbound, respectively, based on the observations by NEOWISE. The dust production rates are 0.01–0.02 kg/sec-1, corresponding to a dust-to-gas production ratio of 2 ≤ fdg ≤ 6. The resulting fractional active area, fA = 3.8±1.9 × 10−5, is the smallest yet reported.[9] The absence of 4.6 μm (W2) excess suggests that 289P/Blanpain contains negligible amounts of CO2 and CO. The perihelion-normalized nongravitational acceleration, a'NG = 3.1 × 10−6, is approximately an order of magnitude smaller than the trend observed for well-studied comets, consistent with weak outgassing.[9]

Exploration proposals

289P/Blanpain has been proposed to be the primary target of the Japanese Next Generation Small-Body Return (NGSR) mission, designed to be launched in the 2030s. The goal of the mission is to return a sample from a comet to Earth, the first time after the Stardust mission. The comet was chosen due to its favorable orbital characteristics and small size.[14] The comet has also been picked as a back-up target for ESA's Comet Interceptor mission,[15] where it is planned to conduct a flyby of the comet by 23 November 2035 if selected.[16]

Source of the Phoenicids

Comet 289P/Blanpain currently has an Earth-MOID of 0.015 AU (2.2 million km; 1.4 million mi).[7] The comet has been proposed as the probable source of the Phoenicid meteor stream, since the first observation of a Phoenicids meteor storm in 1956.[17] Analysis of the orbits of asteroid 2003 WY25 have supported this conjecture, and it is thought likely that the comet was already breaking up at the time of its 1819 return.[18] The 1956 meteor storm was created by trails formed from the late 18th through the early 19th centuries.[19] Elevated Phoenicids activity was also observed on 2 December 2014,[20] when Earth intersected with dust trails created in the early 20th century, indicating that the comet was then active enough to create meteors but not as active as in the early 19th century.[21]

A separate 2025 study expressed doubt in having 289P/Blanpain as the sole true parent body of the Phoenicids,[22] as the comet's nucleus is too small to explain the total mass of the entire meteoroid stream,[8] however debris from two other comets (46P/Wirtanen and 104P/Kowal) may have additionally contributed to it.[22]

Notes

  1. ↑ Observation arc from the Minor Planet Center database only covered dates from 14 December 1819 until 15 July 2024 (204.59 years). This figure included its entire arc up to 28 November 1819.

References

  1. 1 2 G. W. Kronk (2003). Cometography: A Catalog of Comets. Vol. 2: 1800–1899. Cambridge University Press. pp. 51–53. ISBN 978-0-521-58505-7.
  2. 1 2 3 G. V. Williams; H. Sato; B. G. Marsden; et al. (July 2013). D. W. Green (ed.). "Comet P/1819 W1 = 2003 WY25 (Blanpain)" (TXT). Central Bureau for Astronomical Telegrams. 3574: 1. Bibcode:2013CBET.3574....1W.
  3. ↑ J. Ticha; M. Tichy; M. Kocer; et al. (22 November 2003). K. E. Smalley (ed.). "2003 WY25". Minor Planet Electronic Circulars. 2003-W41. Bibcode:2003MPEC....W...41T.
  4. ↑ "Comet Names and Designations". International Comet Quarterly. Retrieved 2 July 2026.
  5. 1 2 "289P/Blanpain Orbit". Minor Planet Center. Retrieved 9 April 2017.
  6. ↑ "Horizons Batch for 289P/Blanpain (90001257) on 2030-Aug-06" (Perihelion occurs when rdot flips from negative to positive). JPL Horizons. Retrieved 10 April 2026.
  7. 1 2 3 4 "289P/Blanpain – JPL Small-Body Database Lookup". ssd.jpl.nasa.gov. Jet Propulsion Laboratory. Retrieved 20 June 2026.
  8. 1 2 3 4 D. C. Jewitt (2006). "Comet D/1819 W1 (Blanpain): Not Dead Yet". The Astronomical Journal. 131 (4): 2327–2331. Bibcode:2006AJ....131.2327J. doi:10.1086/500390.
  9. 1 2 3 4 T. Kasuga (2025). "Comet 289P/Blanpain: Near-perihelion Activity and the Phoenicids". The Astronomical Journal. 169 (2): 54. arXiv:2411.13501. doi:10.3847/1538-3881/ad95fd.
  10. ↑ S. Nakano; G. V. Williams; et al. (7 July 2013). "P/1819 W1 = 2003 WY25 (Blanpain)". Minor Planet Electronic Circulars. 2013-N21. Bibcode:2013MPEC....N...21N.
  11. ↑ S. Foglia; M. Micheli; H. B. Ridley (13 February 2005). D. W. Green (ed.). "Comet D/1819 W1 (Blanpain) and 2003 WY25". IAU Circular. 8485 (1). Bibcode:2005IAUC.8485....1F.
  12. 1 2 Q. Z. Ye; D. L. Clark (2019). "Rising from Ashes or Dying Flash? The Mega Outburst of Small Comet 289P/Blanpain in 2013". The Astrophysical Journal Letters. 878 (2): L34–L40. arXiv:1906.07137. Bibcode:2019ApJ...878L..34Y. doi:10.3847/2041-8213/ab26bc.
  13. ↑ R. J. Wainscoat; M. Micheli; D. Woodworth; et al. (6 July 2013). "2003 WY25". Minor Planet Electronic Circulars. 2013-N20. Bibcode:2013MPEC....N...20W.
  14. ↑ S. Wakita; H. Kurokawa; Y. Shimaki; et al. (18–23 June 2023). The Next Generation Small-Body Sample Return: A Japanese Mission Plan to a Comet (PDF). Asteroids, Comets, Meteors Conference. Vol. 2851. Flagstaff, Arizona. p. 2029.
  15. ↑ G. H. Jones; C. Snodgrass; C. Tubiana; et al. (2024). "The Comet Interceptor Mission" (PDF). Space Science Reviews. 220 (1): 9. Bibcode:2024SSRv..220....9J. doi:10.1007/s11214-023-01035-0. hdl:11577/3505816. PMC 10808369. PMID 38282745.
  16. ↑ M. E. Schwamb; M. M. Knight; G. H. Jones; et al. (2020). "Potential Backup Targets for Comet Interceptor". Research Notes of the American Astronomical Society. 4 (2): 21. arXiv:2002.01744. Bibcode:2020RNAAS...4...21S. doi:10.3847/2515-5172/ab7300.
  17. ↑ H. B. Ridley (1963). "The Phoenicid Meteor Shower of 1956 December 5". Monthly Notes of the Astronomical Society of Southern Africa. 22: 42–49. Bibcode:1963MNSSA..22...42R.
  18. ↑ P. Jenniskens; E. Lyytinen (2005). "Meteor Showers from the Debris of Broken Comets: D/1819 W1 (Blanpain), 2003 WY25, and the Phoenicids". The Astronomical Journal. 130 (3): 1286–1290. Bibcode:2005AJ....130.1286J. doi:10.1086/432469.
  19. ↑ J. Watanabe; M. Sato; T. Kasuga (2005). "Phoenicids in 1956 Revisited". Publications of the Astronomical Society of Japan. 57 (5): L45–L49. Bibcode:2005PASJ...57L..45W. doi:10.1093/pasj/57.5.L45.
  20. ↑ M. Sato; J. Watanabe; C. Tsuchiya; et al. (2017). "Detection of the Phoenicids meteor shower in 2014". Planetary and Space Science. 143: 132–137. Bibcode:2017P&SS..143..132S. doi:10.1016/j.pss.2017.03.010.
  21. ↑ Y. Fujiwara; T. Nakamura; S. Uehara; T. Sagayama; H. Toda (2017). "Optical observations of the Phoenicid meteor shower in 2014 and activity of comet 289P/Blanpain in the early 20th century" (PDF). Publications of the Astronomical Society of Japan. 69 (4): 60–68. Bibcode:2017PASJ...69...60F. doi:10.1093/pasj/psx035.
  22. 1 2 M. Kováčová; L. Neslušan; D. Tomko (2025). "Search for the True Parent Body of the Phoenicid Meteor Shower". The Astronomical Journal. 169 (6): 331–342. Bibcode:2025AJ....169..331K. doi:10.3847/1538-3881/adcf90.
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