Weywot

This article is about the moon. For the Tongva god, see Weywot (mythology).

Weywot
Quaoar and Weywot (left of Quaoar) imaged by the Hubble Space Telescope in 2006
Discovery[1][2]
Discovered by
Discovery date14 February 2006
Designations
Designation
(50000) Quaoar I[4]: 134 
Pronunciation/ˈweɪwɒt/
S/2006 (50000) 1[5]
Orbital characteristics[6]
Epoch 23 March 2008 (JD 2454549.42)[6]
13289±189 km (2023)[7]
13900±200 (2013)[6]
Eccentricity0.056±0.093 (2023)[7]
0.137±0.006 (2013)[6]
12.4311±0.0015 d (2023)[7]
12.4314±0.0002 d (2013)[6]
Inclination15.8°±0.7° (to ecliptic)
1.0°±0.7°
335°±0.7°
Satellite of50000 Quaoar
Physical characteristics
≈ 200 km[8]
Albedo≈ 0.04[8]
24.7[9][a]
≈ 8.3[a]

Weywot (formal designation (50000) Quaoar I; provisional designation S/2006 (50000) 1) is a natural satellite or moon of the trans-Neptunian dwarf planet Quaoar. It was discovered by Michael Brown and Terry-Ann Suer using images taken by the Hubble Space Telescope on 14 February 2006. Named after the Tongva sky god and son of Quaoar, Weywot is thought to be a fragment of Quaoar that was ejected into an eccentric orbit around the dwarf planet by a major impact event billions of years ago. The moon is nearly 200 km (120 mi) in diameter and it orbits Quaoar every 12.4 days at an average distance of 13,300 km (8,300 mi). Weywot is thought to play a role in maintaining Quaoar's outer ring by gravitationally influencing it in an orbital resonance.

Discovery

Weywot was first imaged by the Hubble Space Telescope on 14 February 2006, during Michael Brown's survey for satellites around large trans-Neptunian objects (TNOs) using Hubble's high-resolution Advanced Camera for Surveys.[1][10] Consecutive images from that date showed that Weywot appeared stationary relative to Quaoar and was visibly separated at an angular distance of 0.35 arcseconds.[1][11]: 1547  After Brown's Hubble survey concluded in late 2006, he and his colleague Terry-Ann Suer reported their newly discovered TNO satellites to the Central Bureau for Astronomical Telegrams, which published their discovery of Weywot alongside three other TNO satellites on 22 February 2007.[10][1]

To determine Weywot's orbit, Brown reobserved Weywot with Hubble in March 2007 and March 2008.[12][13][9] Together with his colleague Wesley Fraser, Brown published the first preliminary orbit of Weywot in May 2010. Fraser and Brown were unable to precover Weywot in earlier ultraviolet Hubble images of Quaoar from 2002, either because the satellite was obscured by Quaoar or it was too faint in ultraviolet light.[11]: 1548 

Name

Upon discovery, Weywot was given a provisional designation, S/2006 (50000) 1.[5] Brown left the choice of a name up to the Tongva, whose creator-god Quaoar had been named after. The Tongva chose the sky god Weywot, son of Quaoar.[14] The name of Weywot was officially announced by the Minor Planet Center in a notice published on 4 October 2009.[4]: 134 

Orbit

Orbit diagrams of the Quaoar–Weywot system
Viewed from Earth
Viewed top-down over Quaoar's north pole

Weywot orbits Quaoar at an average distance of 13,300 km (8,300 mi) and takes 12.4 days to complete one revolution.[7]: 3  Its orbit is likely coplanar with Quaoar's equator,[15]: 1  while the entire Quaoar system is inclined by about 16° with respect to the ecliptic plane.[6]: 359 

Weywot has a high orbital eccentricity of 0.14, which challenges theoretical expectations that Weywot could have formed out of a disk of material in circular orbit around Quaoar.[6]: 361  Instead of having a synchronous rotation tidally locked to Quaoar, Weywot's high eccentricity may subject it to a spin-orbit resonance similar to the planet Mercury, where its rotation period is an integer ratio of its orbital period.[6]: 361  Several possible explanations for Weywot's high eccentricity include collisions with other bodies, an origin as a collisionally-ejected fragment of Quaoar, gravitational perturbations, or resonances by other massive bodies.[6]: 362  Of these scenarios, Weywot most likely formed as a fragment of Quaoar that was ejected into an initially eccentric orbit by a major impact event billions of years ago. Weywot's orbit must have tidally evolved very slowly for it to remain eccentric today, which would mean its orbit has changed very little since it had formed.[6]: 362 [16] The trans-Neptunian dwarf planet 225088 Gonggong hosts a similarly eccentric satellite named Xiangliu, and it is inferred to have formed and evolved in the same way as Weywot.[16]

Prior to further observations in 2019, orbit determinations for Weywot were complicated by the issue of mirror ambiguity, where two possible inclinations could equally fit Weywot's orbit due to the lack of parallactic change in its projected orbital plane.[6]: 359 [11]: 1548–1549  That is, it could not be recognized whether Weywot orbited prograde or retrograde with respect to the ecliptic. The discontinuity of known observations of Weywot at the time also resulted in a 0.39-day alias in its orbital period, which allowed for even more possible orbit solutions with different orbital periods.[6]: 359  These issues were eventually resolved when astronomers obtained a precise measurement of Weywot's position from a stellar occultation on 4 August 2019, which allowed researchers to unambiguously settle on a prograde 12.4-day orbit for Weywot.[7]: 6 

Ring dynamics

In February 2023, astronomers announced the discovery of a distant ring orbiting Quaoar at a distance of 4,148 km (2,577 mi), which nearly coincides with the 6:1 mean-motion orbital resonance with Weywot that lies slightly interior to the ring at 4,021 km (2,499 mi).[7]: 3  This near-coincidence suggests Weywot could play a role in perturbing the ring by producing irregularities in the ring's width and density. Together with Quaoar's 1:3 spin-orbit resonance that lies slightly farther from the ring, the 6:1 Weywot mean-motion resonance is thought to help prevent the ring from accreting into a solid body.[7]: 6  It is unknown which of these two resonances plays a more dominant role in maintaining the ring, as the underlying parameters necessary to calculate their effects are poorly known.[7]: 6  The ring is likely coplanar with Weywot's orbit within a relative inclination of 5°±7°.[15]: 4 

Physical characteristics

Weywot is extremely dim, with an apparent magnitude of 24.7—that is, 5.6±0.2 magnitudes fainter than Quaoar in visible light.[1][9] Combined with its close proximity to Quaoar, Weywot's faintness makes observations difficult, leaving it resolvable only to the most sensitive telescopes such as the Hubble Space Telescope and the Keck Telescopes.[10] For these reasons, most of Weywot's physical properties such as its mass, color, and light curve have yet to be measured.[11]: 1547 

As of 2023, Weywot is thought to be about 200 km (120 mi) in diameter, based on multiple observations of a stellar occultation by Weywot on 22 June 2023.[8] Occultations by Weywot have been observed previously on 4 August 2019, 11 June 2022, and 26 May 2023, which all gave similar diameter estimates of about 170 km (110 mi).[17][18][8] Given Weywot's magnitude difference from Quaoar, this occultation-derived diameter suggests Weywot has low geometric albedo of about 0.04, considerably darker than Quaoar's albedo of 0.12.[8] Weywot was previously thought to have a diameter of 81 ± 11 km (50 ± 7 mi), about half that of the occultation measurement, because researchers based this estimate only on Weywot's relative brightness and assumed it had a similar albedo as Quaoar.[19]: 15 [11]: 1547 [8]

Notes

  1. ^ a b Weywot is 5.6±0.2 magnitudes fainter than Quaoar in visible wavelengths.[1][2] The apparent magnitude of Weywot by itself is the sum of this magnitude difference and Quaoar's apparent magnitude of 19.0. Likewise, the absolute magnitude of Weywot is the sum of this magnitude difference and Quaoar's absolute magnitude of 2.74.[9]

References

  1. ^ a b c d e f Green, Daniel W. E. (22 February 2007). "Satellites of 2003 AZ_84, (50000), (55637), and (90482)". IAU Circular (8812). Central Bureau for Astronomical Telegrams: 1. Bibcode:2007IAUC.8812....1B. Archived from the original on 19 July 2011. Retrieved 5 July 2011.
  2. ^ a b Johnston, Wm. Robert (21 September 2014). "(50000) Quaoar and Weywot". Asteroids with Satellites Database. Johnston's Archive. Retrieved 26 May 2009.
  3. ^ Suer, Terry-Ann. "Publications". sites.google.com. Retrieved 11 February 2023.
  4. ^ a b "M. P. C. 67220" (PDF). Minor Planet Circulars (67220). Minor Planet Center: 134. 4 October 2009. Retrieved 12 February 2023.
  5. ^ a b "JPL Small-Body Database Browser: 50000 Quaoar (2002 LM60)". Jet Propulsion Laboratory. Retrieved 11 February 2023.
  6. ^ a b c d e f g h i j k l Fraser, Wesley C.; Batygin, Konstantin; Brown, Michael E.; Bouchez, Antonin (January 2013). "The mass, orbit, and tidal evolution of the Quaoar-Weywot system". Icarus. 222 (1): 357−363. arXiv:1211.1016. Bibcode:2013Icar..222..357F. doi:10.1016/j.icarus.2012.11.004. S2CID 17196395.
  7. ^ a b c d e f g h B. E. Morgado; B. Sicardy; F. Braga-Ribas; J. L. Ortiz; H. Salo; F. Vachier; et al. (8 February 2023). "A dense ring of the trans-Neptunian object Quaoar outside its Roche limit". Nature. 614 (7947): 239–243. Bibcode:2023Natur.614..239M. doi:10.1038/S41586-022-05629-6. ISSN 1476-4687. Wikidata Q116754015.
  8. ^ a b c d e f Fernandez-Valenzuela, E.; Holler, B.; Ortiz, J. L.; Vachier, F.; Braga-Ribas, F.; Rommel, F.; et al. (October 2023). Weywot: the darkest known satellite in the trans-Neptunian region. 55th Annual DPS Meeting Joint with EPSC. Vol. 55. San Antonio, Texas. 202.04.
  9. ^ a b c d Grundy, Will (21 March 2022). "Quaoar and Weywot (50000 2002 LM60)". www2.lowell.edu. Lowell Observatory. Retrieved 11 February 2023.
  10. ^ a b c Brown, Michael (July 2005). "Icy planetoids of the outer solar system". Mikulski Archive for Space Telescopes. Space Telescope Science Institute: 10545. Bibcode:2005hst..prop10545B. Cycle 14. Retrieved 11 February 2023.
  11. ^ a b c d e Fraser, Wesley C.; Brown, Michael E. (May 2010). "Quaoar: A Rock in the Kuiper Belt" (PDF). The Astrophysical Journal. 714 (2): 1547–1550. arXiv:1003.5911. Bibcode:2010ApJ...714.1547F. doi:10.1088/0004-637X/714/2/1547. S2CID 17386407.
  12. ^ Brown, Michael (July 2006). "The largest Kuiper belt objects". Mikulski Archive for Space Telescopes. Space Telescope Science Institute: 10860. Bibcode:2006hst..prop10860B. Cycle 15. Retrieved 27 April 2023.
  13. ^ Brown, Michael (July 2007). "Collisions in the Kuiper belt". Mikulski Archive for Space Telescopes. Space Telescope Science Institute: 11169. Bibcode:2007hst..prop11169B. Cycle 16. Retrieved 27 April 2023.
  14. ^ Street, Nick (August 2008). "Heavenly Bodies and the People of the Earth". Search Magazine. Heldref Publications. Archived from the original on 18 May 2009. Retrieved 8 January 2020.
  15. ^ a b C. L. Pereira; B. Sicardy; B. E. Morgado; F. Braga-Ribas; E. Fernández-Valenzuela; D. Souami; et al. (2023). "The two rings of (50000) Quaoar". Astronomy & Astrophysics. arXiv:2304.09237. Bibcode:2023A&A...673L...4P. doi:10.1051/0004-6361/202346365. ISSN 0004-6361. Wikidata Q117802048.
  16. ^ a b Arakawa, Sota; Hyodo, Ryuki; Shoji, Daigo; Genda, Hidenori (December 2021). "Tidal Evolution of the Eccentric Moon around Dwarf Planet (225088) Gonggong". The Astronomical Journal. 162 (6): 29. arXiv:2108.08553. Bibcode:2021AJ....162..226A. doi:10.3847/1538-3881/ac1f91. S2CID 237213381. 226.
  17. ^ Kretlow, Mike (January 2020). "Beyond Jupiter – (50000) Quaoar" (PDF). Journal for Occultation Astronomy. 10 (1). International Occultation Timing Association: 24–31. Bibcode:2020JOA....10a..24K.
  18. ^ "2022 Asteroidal Occultation Preliminary Results – 50000(1) Weywot 2022 Jun 11". www.asteroidoccultation.com. International Occultation Timing Association. 11 June 2022. Archived from the original on 12 February 2023.
  19. ^ Fornasier, S.; Lellouch, E.; Müller, T.; Santos-Sanz, P.; Panuzzo, P.; Kiss, C.; et al. (July 2013). "TNOs are Cool: A survey of the trans-Neptunian region. VIII. Combined Herschel PACS and SPIRE observations of nine bright targets at 70-500 µm". Astronomy and Astrophysics. 555: 22. arXiv:1305.0449v2. Bibcode:2013A&A...555A..15F. doi:10.1051/0004-6361/201321329.