Astronomy:120347 Salacia

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120347 Salacia 24px or 24px (rare)
Keck Telescope image of Salacia (center) and its moon Actaea (left), taken by the NIRC2 near-infrared camera on 3 August 2010.
Discovery[1][2]
Discovered byH. G. Roe
M. E. Brown
K. M. Barkume
Discovery sitePalomar Obs.
Discovery date22 September 2004
Designations
(120347) Salacia
Pronunciation/səˈleɪʃə/ (sə-LAY-shə)
Named afterSalacia (Roman mythology)[2]
2004 SB60
Minor planet categoryTNO[1] · classical (hot)[3]
extended[4]
AdjectivesSalacian
Orbital characteristics[1]
Epoch 31 May 2020 (JD 2459000.5)
Uncertainty parameter 3
Observation arc37.16 yr (13,572 days)
Earliest precovery date25 July 1982
|{{{apsis}}}|helion}}46.670 AU
|{{{apsis}}}|helion}}37.697 AU
42.184 AU
Eccentricity0.10636
Orbital period273.98 yr (100,073 days)
Mean anomaly123.138°
Mean motion0° 0m 12.951s / day
Inclination23.921°
Longitude of ascending node279.880°
312.294°
Known satellites1 (Actaea)
Physical characteristics
Mean diameter
Mass4.861+0.076
−0.074×1020 kg (Total system mass)[8]
Mean density≈1.45 g/cm3 (7 September 2025)[lower-alpha 2][5]
1.38+0.18
−0.22 g/cm3 (2 September 2025)[lower-alpha 3][8]
1.50±0.12 g/cm3 (2019)[6]
1.26±0.16 g/cm3 (2017)[7]
Sidereal rotation period5.49403±0.00016 d (synchronous)[8]
Geometric albedo0.041±0.004 (2025)[5]
0.042±0.004 (2017)[7]
Apparent magnitude20.7
Absolute magnitude (H)4.360±0.011 (Salacia+Actaea)[3]
4.476±0.013 (Salacia)[3]
4.15[1]


120347 Salacia (provisional designation 2004 SB60) is a large trans-Neptunian object in the Kuiper belt. It was discovered on 22 September 2004 by American astronomers Henry G. Roe, Michael E. Brown, and Kristina Barkume using the Hale Reflector at the Palomar Observatory.[2][11] Its discovery was officially announced in May 2005.[11] Salacia orbits the Sun at an average distance slightly greater than that of Pluto, and is classified as a hot cubewano or a scattered–extended object.[3][12] It was named after the Roman sea goddess Salacia.

Salacia is a possible dwarf planet with an estimated diameter of 838±44 km,[5] and a low light curve, implying a nearly spherical shape.[8] While older size estimates suggested a low density and highly porous interior,[7] newer measurements calculate a higher density between 1.45 g/cm3 and 1.50±0.12 g/cm3.[5][6] It has a dark gray surface with a neutral color index and an exceptionally low albedo of 0.041±0.004.[5][10] This low albedo indicates a lack of geological activity.[6] Observations by the James Webb Space Telescope (JWST) showed that water ice makes up less than 5% of its surface, detecting both amorphous and crystalline water ice alongside carbon dioxide ice.[9][13] It lacks volatile super-ices like methane, placing it in the "prominent water" (H2O-type) TNO group alongside objects like 307261 Máni and 90482 Orcus.[9]: 4 

Salacia has one known moon, Actaea, and their combined system mass is 4.861+0.076
−0.074×1020 kg.[8] The primary body and its moon form a fully tidally locked system with a synchronous rotation period of 5.49 days, similar to the Pluto–Charon system.[8] The two bodies will pass directly in front of each other during a rare mutual occultation season starting in 2067.[3]

History

Discovery

The dome of the Palomar Observatory in California, where Salacia was discovered on 22 September 2004.[11]

Salacia was discovered on 22 September 2004 by American astronomers Henry Roe, Michael Brown, and Kristina Barkume at the Palomar Observatory in California, United States.[2] The discovery observations were formally published in May 2005 in the Minor Planet Electronic Circular (MPEC) 2005-J26.[11] The object was announced alongside a group of seven new trans-Neptunian objects tracked by the IAU's Minor Planet Center.[11]

At the time of its initial detection on 22 September, Salacia was recorded with a red-filter apparent magnitude ranging between 20.1 and 20.6.[11] Following its initial tracking, the object was assigned the provisional designation 2004 SB60.[2] While the discovery tracking occurred in 2004, astronomers successfully verified earlier positions of the body through archival precovery images taken at the Siding Spring Observatory (Station 260) dating back to 25 July 1982.[2][14]

Further observations

The observation arc of Salacia begins with a precovery observation on 25 July 1982 at the Siding Spring Observatory (Station 260).[2] Between 2001 and 2003, Salacia was pictured multiple times by the Near-Earth Asteroid Tracking (NEAT) program at Palomar (Station 644) and the Sloan Digital Sky Survey at Apache Point (Station 645).[2] After its discovery in 2004,[2] it was observed by the 5-meter Hale Reflector (Station 675) and the 3.5-meter telescope at Mauna Kea (Station 568).[11] As of May 2026, a total of 490 observations have been recorded over a period of 37.16 years (13,572 days).[1] These observations were made by ground-based and space-based telescopes, such as the Hubble Space Telescope (Station 250).[2] More recent tracking was done by the Pan-STARRS 1 survey (Station F51), the Weizmann Astrophysical Observatory (Station M01), and the Pises Observatory (Station 122).[2] The most recent observation recorded in the Minor Planet Center database was done on 1 November 2025, at F51 – Pan-STARRS 1, Haleakalā.[2]

Nomenclature

Numbering and naming

Salacia, the goddess of salt water

This minor planet was named after Salacia (/səˈleɪʃə/ sə-LAY-shə, la), the goddess of salt water consort of Neptune.[15][16][17][18][19] She is the Roman equivalent of the Greek sea goddess Amphitrite or Tethys.[20][2] The object had been assigned its permanent minor planet number (120347) on 16 November 2005, following the precise consolidation of its orbital path data.[14] The official naming citation was subsequently published on 18 February 2011 in M.P.C. 73984, which formally established the name within the International Astronomical Union's minor planet index.[21] Its moon's name is called Actaea (/ækˈtiːə/; Ancient Greek: Ἀκταία, romanized: Aktaía, lit. 'the dweller on coasts'.[22] It was from Ancient Greek: ἀκτή, romanized: akté, lit. 'seashore' or 'rocky shore') being one of the 50 Nereid sea-nymphs, matching the system's marine naming theme.[23][24]

Planetary symbol

Salacia's symbol

Planetary symbols are no longer used much in astronomy, so Salacia never received a symbol in the astronomical literature. Denis Moskowitz, a software engineer who designed most of the dwarf planet symbols, proposed a stylised hippocamp (16px, formerly 16px) as the symbol for Salacia;[25][26] although this symbol is not widely used.

Orbit and classification

Salacia orbits the Sun at a distance of 37.7–46.7 AU with a semi-major axis of 42.2 AU, finishing its orbit once every 274.0 years.[1] Salacia is a non-resonant object with a moderate eccentricity of approximately 0.11 and a large inclination of 23.9° with respect to the ecliptic.[1] The orbit of Salacia is similar to Pluto's, except for a near opposite longitude of ascending node. Its current position is near its most northern position above the ecliptic.

Salacia is located in the classical region of the Kuiper belt between 39 and 48 AU from the Sun.[3] Because it lacks an active orbital resonance with Neptune, it is grouped as a typical member of the classical Kuiper belt population, commonly called "cubewanos".[3] However, Salacia's steep orbital inclination of 23.9° places it within the dynamically "hot" sub-population of the classical belt.[1][3] Unlike cold classical objects that formed in place along circular paths, hot classical bodies likely formed closer to the Sun and were scattered outward into highly tilted orbits during the early migration of Neptune.[27]: 230 

Astronomers utilize different frameworks to sort these outer Solar System bodies, leading to a long-standing academic debate over Salacia's exact status.[12] In the Deep Ecliptic Survey framework by Elliot et al., Salacia is grouped as a scattered–extended object because the system automatically places highly tilted orbits into the scattered categories.[12] Conversely, Brett Gladman and his team reject this label based on a 10-million-year computer simulation testing orbital stability.[12] Because Salacia's orbit stays perfectly stable and completely clear of Neptune's gravity during the simulation, Gladman et al. formally classify it as a hot classical Kuiper belt object.[12] This orbital path also places it near the Haumea collisional family by coincidence; however, tracking and space-based spectral data confirm Salacia is an unrelated background object despite its water-ice rich surface.[3][9]

The orbit of Salacia compared to Pluto's and the eight planets' orbits in top view and the side view.

Observability

Occultations

Salacia stellar occultations
Date Star apparent magnitude (G-mag) Occultation
duration		 Measured chord
length		 Target body Observing asset /
Network
27 Dec 2018 15.5 66.7 s (maximum duration) Maybe Salacia LESIA Lucky Star[28]
28 Jul 2023 Maybe 31.2±0.3 s 786.5±7.8 km Salacia La Silla 1.54m Telescope[29]: 3 
17 Aug 2024 15.9 48.2 s (maximum duration) Maybe Salacia & Actaea Hubble / LESIA[30][31]
26 Jan 2027 13.9 42.5 s (predicted) Maybe Salacia SwRI RECON network[32]

Stellar occultations by Salacia happen when it passes in front of a background star, letting scientists measure its precise position, shape, and size profile.[33]: 1  To make predictions more precise, astronomers map Salacia's orbit using wide-field star catalogs, while a 2015 study identified four potential occultations visible by the James Webb Space Telescope using faint background stars between infrared magnitudes 14 and 16.[34][35] Several recorded campaigns have progressively narrowed Salacia's orbital path from an early uncertainty of about 2300 km.[34] On 27 December 2018, an event monitored by the LESIA - Observatoire de Paris against a Gaia magnitude 15.5 star captured a 4.8 magnitude drop, significantly refining the orbit from an initial ground-based uncertainty of 4214.9 km.[28] Following this, a 28 July 2023 occultation captured by the 1.54m Danish Telescope at La Silla recorded a light drop lasting 31.2±0.3 s at a relative speed of 25.24 km/s, providing a direct single-chord surface size measurement of 786.5±7.8 km.[29]: 2–3  A rare double stellar occultation was recorded on 17 August 2024, when both Salacia and its moon, Actaea, blocked the same Gaia magnitude 15.9 star within 5 minutes of each other.[31][30] Because the initial ground-based path carried a massive uncertainty of 1842.8 km, astronomers used the Hubble Space Telescope under Proposal 17848 to take precise photos beforehand, reducing the uncertainty to just 300 km.[30]: 1–2  This allowed ground stations to align their telescopes perfectly, recording a sharp 5.0 magnitude drop to measure both bodies, while the RECON network is targeting a future occultation of a magnitude 13.9 star scheduled for 26 January 2027.[31][30][32]

Rotation and hypothesized shape

Light curves and shape

Salacia's light curve amplitude.

Salacia has a very low light curve amplitude of only about 3%, meaning its brightness does not change much as it spins.[3] Accurate tracking measures this variation at 0.0900±0.0036 magnitudes.[8] This small change suggests that Salacia is either nearly a perfect sphere or its pole is pointing almost directly at Earth.[8]

In planetary science, minor light variations can be caused by either an elongated shape or by dark and light spots on a round body.[8] An elongated shape would produce a double-peaked light curve with two minimums and maximums per rotation.[8] Because Salacia's light variations show a single-peaked pattern with only one peak per cycle, astronomers explicitly reject the elongated triaxial ellipsoid shape idea.[8] Instead, the light curve is entirely driven by uneven albedo variations across its surface, so Salacia is unlikely to be an elongated triaxial ellipsoid, but rather having a nearly spherical shape with small albedo variations across its surface.[8]

Rotational speed and mutual tidal locking

In 2014, early studies estimated that Salacia rotated very fast, once every 6.09–6.5 hours.[1][36] However, a long-term study published in 2025 showed this was a mathematical error called "observational aliasing."[8] Because ground telescopes could only watch Salacia for a few days at a time, the gaps in the data made a slow 5.49-day spin look like a fast 6.5-hour cycle.[8]

The 2025 study analyzed 165 hours of data collected over 16 years.[8] By combining ground tracking with images from the Hubble Space Telescope, scientists found that Salacia's 5.49-day rotation exactly matches the time its moon, Actaea, takes to complete one orbit (5.49389±0.00001 d).[8]

The Pluto–Charon system — an example of mutual tidal locking, similar to the Salacia–Actaea system.

This means the two bodies are mutually tidally locked in a "doubly synchronous rotation," always showing the exact same face to each other just like Pluto and Charon.[8] Before this happened, Salacia likely spun much faster, at around 10 hours per rotation.[8] Because Actaea is relatively large, its gravitational pull created internal friction that gradually slowed Salacia down.[8] Computer models show this tidal slowing took only 150 million to 400 million years to finish, meaning the pair has been locked in this balance for billions of years.[8]

Separating the individual light data also revealed features about the moon itself.[8] While Salacia shows small brightness changes, Actaea exhibits a very high light curve amplitude of at least 0.95 magnitudes.[8] This indicates that Actaea either has a highly stretched shape or extreme surface contrasts with large dark and light patches.[8] This discovery cements the system as only the third confirmed doubly synchronous binary in the trans-Neptunian region, joining Pluto–Charon and Eris–Dysnomia.[8]

Physical characteristics

Comparison of sizes, albedos, and colors of various large trans-Neptunian objects with diameters greater than 700 km (430 mi). Salacia is shown on the middle row, third from the right. The dark colored arcs represent uncertainties of the object's size.

Size, mass and density

Template:Section needs expansion

History of diameter estimates for Salacia
Year of Publication Diameter (km) Method References
2012 905±103 thermal (Spitzer) [37]
2013 874±32 thermal (Herschel) [38]
2013 854±45 thermal (Spitzer) [39]
2017 866±37 dynamical (HST) [7]
2019 846±21 thermal (combined) [6][lower-alpha 4]
2025 838±44 thermal (ALMA/NEATM) [5]

In 2025, the total mass of the Salacia–Actaea system was estimated to be at 4.861+0.076
−0.074×1020 kg,[8] with an average system density of 1.50±0.12 g/cm3 which was estimated in 2019;[6] Salacia itself was estimated to be around 838 km in diameter,[5] which is slightly smaller than Orcus (910+50
−40 km).[40] Salacia has the lowest albedo of any known large trans-Neptunian object,[3] having an albedo of only 0.041±0.004.[5] According to the old estimate from 2017 based on an improved thermophysical modelling, the size of Salacia is slightly larger at around 866 km and its density therefore is slightly lower, being calculated at only 1.26 g/cm3 with the old mass estimate of around (4.38±0.16)×1020 kg.[7]

At 838±44 km,[5] Salacia belongs to the proposed class of "mid-sized" TNOs between 400 and 1,000 km (250 and 620 mi) in diameter.[41] It represents the evolutionary transition between small, low-density TNOs and large, high-density dwarf planets.[41] William Grundy and his team originally hypothesized that these mid-sized objects maintain highly porous and unheated interiors because structurally similar bodies like 55637 Uni and 229762 Gǃkúnǁʼhòmdímà exhibit low densities near 1 g/cm³.[41] Under this framework, Grundy et al. proposed that low-albedo, mid-sized bodies did not undergo internal melting or differentiation like Orcus, Quaoar, and Charon.[41]

Salacia's density and albedo compared to the other most likely dwarf planets

Grundy et al. initially rejected Salacia as a dwarf planet due to its older, lower density estimates,[41] describing Salacia as a "dwarf planet–sized TNO."[6] However, just a few months later after they published the low density theory, they backed off that position when newer studies found that Salacia's density is relatively high, around 1.50±0.12 g/cm3,[6] while kiss et al in 2025 yielded a density of 1.45 g/cm3 assuming equal densities for Salacia and Actaea.[5] If these estimates are accurate, then Salacia would have a higher density than Orcus (1.4±0.2 g/cm3).[42] Though its extremely low albedo of 4.1% remains consistent with an ancient surface that lacks the widespread geological activity typical of larger dwarf planets.[5][6]

American astronomer Michael E. Brown considers Salacia nearly certain to be a dwarf planet, placing it at the lower edge of his "nearly certain" ranking tier.[43]

Surface and spectrum

Salacia has a dark gray surface with an extremely low albedo of 0.041±0.004 that was measured by Kiss et al. in 2025,[5] and a B-V color index of approximately 0.66±0.06,[10] which is considered a neutral color.[10] Salacia's infrared spectrum is complex. Earlier studies have detected an abundance of water ice of less than 5% on the surface.[39][44] However, astronomers got a much clearer look at the surface on 31 August 2023 using the Near-Infrared Spectrograph (NIRSpec) on the James Webb Space Telescope.[9]: 2  Observed under Guaranteed Time Observations program 1191, Salacia was at a heliocentric distance of 45.1 au and a phase angle of 0.94°.[9]: 2 

The near-infrared spectrum of Salacia as measured by the James Webb Space Telescope. The spectrum of Salacia suggests crystalline water ice on its surface.[13][9]

The JWST spectrum showed distinct water-ice absorption bands at 1.5, 2, 3, and between 4–5 μm, with a very sharp drop right at 3 μm.[9]: 1, 3  The specific diagnostic band for crystalline water ice at 1.65 μm is weak and difficult to verify.[9]: 3  This indicates that Salacia's surface has a complex mix of both crystalline and amorphous water ice.[9]: 3–4  The shape of the absorption features between 4.5–5.0 μm depends heavily on how these two ice phases are mixed and the size of their ice grains.[9]: 4  Because water ice has a very high extinction coefficient at 3 μm, the absorption band at that wavelength is nearly 100% optically saturated.[9]: 7  Minor variations in this saturated band suggest the ice sits in complex vertical layers or uneven mixtures in the upper crust.[9]: 7  It also detected carbon dioxide ice through its strong ν3 fundamental vibrational band at 4.25 μm.[9]: 1, 4  The spectrum displays a distinct V-shaped CO2 absorption feature that bottoms out at 4.27 μm.[9]: 4, 8  This specific V-shape shows that the carbon dioxide ice is not a pure crystalline layer, but is likely trapped as an amorphous mixture inside the surrounding water ice.[9]: 8  Data from the 2.6–2.8 μm range showed no signatures of hydrogen peroxide (H2O2), which space radiation usually creates on pure water ice.[9]: 8  Astronomers also searched for a weaker absorption band at 4.37 μm from the heavier isotope 13CO2, but the data was too noisy to confirm it.[9]: 4 

Salacia completely lacks volatile super-ices like methane (CH4) or carbon monoxide (CO).[9]: 1, 5  Its surface escape velocity is only 385–542 m/s, which is too weak to keep solar-heated volatile gases from escaping into space at local temperatures of 30–50 K.[9]: 5  This low gravity explains why Salacia also lacks aliphatic hydrocarbons and complex organic signatures between 3.3–3.6 μm.[9]: 5  However, because Salacia is larger than the critical geophysical threshold of roughly 500 km, it had enough early radiogenic heating to melt and move its internal water and carbon dioxide ices up to the surface.[9]: 7  This internal evolution explains why Salacia keeps an ice-rich surface despite its low albedo and lack of ongoing cryovolcanism.[9]: 7  Because of these strong water and carbon dioxide ice signatures and lack of complex organics, Salacia is classified as a "prominent water" (H2O-type) TNO under recent taxonomic frameworks.[9]: 1, 4  Other mid to large trans-Neptunian objects such as 307261 Máni, 90482 Orcus and 208996 Achlys also have Salacia's neutral spectrum and has a water ice-rich surface or composition. These objects are all classified as "prominent water" (H2O)-type TNOs according to Wong.[9]: 5–6 

Binary system

Moon

Main article: Astronomy:Actaea (moon)
A simulated nearly circular orbit of Actaea at a distance of 5700+30
−29 km away from Salacia.[8]

Salacia has one known moon, Actaea. It orbits Salacia every 5.49389±0.00016 d at a distance of 5700+30
−29 km[8] with an eccentricity of 0.008±0.003.[8] It was discovered on 21 July 2006 by Keith Noll, Harold Levison, Denise Stephens and William Grundy with the Hubble Space Telescope.[45]

Actaea has a diameter of 393±33 km,[5] making it the fifth-largest known moon of a trans-Neptunian object, after Charon (1212±1 km),[46] Dysnomia (615+60
−50 km),[47]: 7  Vanth (442.5±10.2 km),[48] and Ilmarë (403±40 km).[5] Assuming that Actaea has a density of 0.7 g/cm3, which is thought to be typical that of trans-Neptunian objects' moons,[5] The mass ratio between Actaea and Salacia will be approximately 0.044:1.[5][lower-alpha 5] It has an extremely low albedo of 0.021±0.004, which is only half the albedo of Salacia (0.041±0.004).[5]

Tidal evolution

The Salacia system has undergone enough tidal evolution to circularize its orbit, which matches the low measured eccentricity.[8] The ratio of Actaea's semi-major axis to its primary's Hill radius is 0.0023, making it the tightest out of every known trans-Neptunian binary with a calculated orbit.[3]

Tidal forces transferred angular momentum from Salacia's rotation directly into Actaea's orbit, forcing the moon to push farther away until the distance between the two bodies expanded to its modern value of about 13.2 Salacia radii.[8] Tidal models show that if Salacia remained an unheated, mixed-up blend of primitive rock and ice, this evolution would have dragged out for nearly 1 billion years.[8] However, the system could have synchronized much faster, in about 100 million years, if its interior separated early in its history through an ancient, brief epoch of internal melting.[8] This allowed the system to reach its stable, quiet state early in the history of the Solar System, whereas larger, more massive bodies like Eris required nearly 4 billion years to complete their tidal cycles.[8]

Proposed explorations

Salacia has not been visited by a space probe, though many studies have found it to be a feasible target for future missions.[49] Planetary scientists advocate for the exploration of large trans-Neptunian objects to provide insights into the formation and evolution of the Solar System.[50]: 5 

Several studies have analyzed flyby trajectories to Salacia using planetary gravity assists to reduce flight time. A 2019 study by Amanda Zangari and her team showed that a spacecraft launched between 2025 and 2027 could use a single Saturn gravity assist to reach Salacia in 15.4 to 24.2 years, depending on the launch vehicle's power.[49] For later windows, Samuel Walters and James Lyne identified a 2031 trajectory that utilizes an unpowered Jupiter gravity assist, allowing a probe to complete its outer Solar System transit in exactly 25 years and arrive at Salacia in February 2056.[51]: 12 

Advanced flight frameworks using an Earth and Jupiter gravity assist combination (ΔVEGA-JGA) have also been evaluated. A 2021 trajectory survey by James Evans Lyne and colleagues identified a launch window on 15 January 2029 with an 18.4-year transit time, and a second option on 27 February 2042 with an 18.2-year duration.[52]: 2  Multi-target missions involving other outer planets have also been proposed. Bryan J. Holler and his team found a 2040 mission design that performs a close flyby of Neptune before reaching Salacia in December 2046.[50]

A separate dual-probe mission analyzed by Anderson et al. proposed launching an 800 kg Salacia flyby probe alongside a Neptune flagship mission on 28 February 2042.[53]: 39  Under this optimized flight plan, the Salacia probe would use a Jupiter gravity assist to complete its transit in 17.6 years, executing its close flyby encounter in October 2059.[53]: 39  Additionally, the feasibility of an orbital capture rendezvous has been studied, with a 2013 university assessment showing options for putting a 100 to 380 kg orbiter into a permanent orbit around Salacia using a Jupiter swingby.[54]

See also

Notes

  1. ↑ approximation if Salacia and Actaea were both spherical and had the same albedo
  2. ↑ assuming equal densities for the both objects
  3. ↑ assuming equal densities for the both bodies, using the old size estimate of 866±37 km and 290±21 km for Salacia and Actaea respectively.
  4. ↑ approximation if Salacia and Actaea were both spherical and had the same albedo
  5. ↑ This means Actaea is approximately 4.4% the mass of Salacia.

References

  1. ↑ 1.0 1.1 1.2 1.3 1.4 1.5 1.6 1.7 1.8 "JPL Small-Body Database Browser: 120347 Salacia (2004 SB60)". Jet Propulsion Laboratory. 7 November 2019. https://ssd.jpl.nasa.gov/sbdb.cgi?sstr=2120347. 
  2. ↑ 2.00 2.01 2.02 2.03 2.04 2.05 2.06 2.07 2.08 2.09 2.10 2.11 2.12 "(120347) Salacia = 2004 SB60". Minor Planet Center. https://www.minorplanetcenter.net/db_search/show_object?object_id=120347. 
  3. ↑ 3.00 3.01 3.02 3.03 3.04 3.05 3.06 3.07 3.08 3.09 3.10 3.11 Stansberry, J.A. et al. (2012). "Physical Properties of Trans-Neptunian Binaries (120347) Salacia–Actaea and (42355) Typhon–Echidna". Icarus 219 (2): 676–688. doi:10.1016/j.icarus.2012.03.029. Bibcode: 2012Icar..219..676S. 
  4. ↑ Buie, Marc W.. "Orbit Fit and Astrometric record for 120347". SwRI (Space Science Department). http://www.boulder.swri.edu/~buie/kbo/astrom/120347.html. 
  5. ↑ 5.00 5.01 5.02 5.03 5.04 5.05 5.06 5.07 5.08 5.09 5.10 5.11 5.12 5.13 5.14 5.15 5.16 5.17 Kiss, Csaba; Gabányi, Krisztina; Moór, Attila; Müller, Thomas; Fernandez-Valenzuela, Estela; Moullet, Arielle (September 2025). "ALMA submm measurements of the trans-Neptunian binary system satellites Ilmarë, Actaea, Hi'iaka and Namaka". EPSC-DPS Joint Meeting 2025. 18. doi:10.5194/epsc-dps2025-905. https://meetingorganizer.copernicus.org/EPSC-DPS2025/EPSC-DPS2025-905.html. 
  6. ↑ 6.0 6.1 6.2 6.3 6.4 6.5 6.6 6.7 6.8 Grundy, W. M.; Noll, K. S.; Roe, H. G.; Buie, M. W.; Porter, S. B.; Parker, A. H.; Nesvorný, D.; Benecchi, S. D. et al. (2019). "Mutual Orbit Orientations of Transneptunian Binaries". Icarus 334: 62–78. doi:10.1016/j.icarus.2019.03.035. ISSN 0019-1035. Bibcode: 2019Icar..334...62G. http://www2.lowell.edu/~grundy/abstracts/preprints/2019.TNB_orbits.pdf. Retrieved 2019-10-26. 
  7. ↑ 7.0 7.1 7.2 7.3 7.4 7.5 Brown, Michael E.; Butler, Bryan J. (20 June 2017). "The Density of Mid-sized Kuiper Belt Objects from ALMA Thermal Observations". The Astronomical Journal 154 (1): 19. doi:10.3847/1538-3881/aa6346. Bibcode: 2017AJ....154...19B. 
  8. ↑ 8.00 8.01 8.02 8.03 8.04 8.05 8.06 8.07 8.08 8.09 8.10 8.11 8.12 8.13 8.14 8.15 8.16 8.17 8.18 8.19 8.20 8.21 8.22 8.23 8.24 8.25 8.26 8.27 8.28 8.29 8.30 8.31 8.32 Collyer, Cameron; Fernandez-Valenzuela, Estela; Jose Luis Ortiz; Holler, Bryan J.; Proudfoot, Benjamin; Morales, Nicolas; Morales, Rafael; Benecchi, Susan et al. (2025). "Synchronous Rotation in the (120347) Salacia-Actaea System". The Planetary Science Journal 6 (11): 270. doi:10.3847/PSJ/ae0b6a. Bibcode: 2025PSJ.....6..270C. 
  9. ↑ 9.00 9.01 9.02 9.03 9.04 9.05 9.06 9.07 9.08 9.09 9.10 9.11 9.12 9.13 9.14 9.15 9.16 9.17 9.18 9.19 9.20 9.21 9.22 9.23 9.24 Wong, IanExpression error: Unrecognized word "etal". (December 2025). "JWST/NIRSpec Observations of Salacia-Actaea and Máni: Exploring Population-level Trends among Water-ice-rich Kuiper Belt Objects". The Planetary Science Journal 6 (12): 281. doi:10.3847/PSJ/ae1d63. Bibcode: 2025PSJ.....6..281W. 
  10. ↑ 10.0 10.1 10.2 10.3 10.4 10.5 Belskaya, Irina N.; Barucci, Maria A.; Fulchignoni, Marcello; Lazzarin, M. (April 2015). "Updated taxonomy of trans-neptunian objects and centaurs: Influence of albedo". Icarus 250: 482–491. doi:10.1016/j.icarus.2014.12.004. Bibcode: 2015Icar..250..482B. 
  11. ↑ 11.0 11.1 11.2 11.3 11.4 11.5 11.6 "MPEC 2005-J26: SEVEN TNOS". Minor Planet Center. 2026-05-10. https://www.minorplanetcenter.net/mpec/K05/K05J26.html. 
  12. ↑ 12.0 12.1 12.2 12.3 12.4 Gladman, B.; Marsden, B. G.; VanLaerhoven, C. (2008). "Nomenclature in the Outer Solar System". The Solar System Beyond Neptune. p. 43. http://www.lpi.usra.edu/books/ssbn2008/7002.pdf. Retrieved 2016-05-01. 
  13. ↑ 13.0 13.1 Cook, J. C.; Brunetto, R.; De Souza Feliciano, A. C.; Emery, J.; Holler, B.; Parker, A. H. (June 2023). "Hapke Modeling of Several KBOs from JWST Observations". Asteroids, Comets, Meteors Conference 2023. Lunar and Planetary Institute. https://www.hou.usra.edu/meetings/acm2023/pdf/2526.pdf. Retrieved 2023-05-24. 
  14. ↑ 14.0 14.1 Johnston, Wm. Robert (2026-05-10). "(120347) Salacia and Actaea". Johnston's Archive. https://www.johnstonsarchive.net/astro/astmoons/am-120347.html. 
  15. ↑ Gurney, Hudson (2008). The Works of Apuleius, Comprising the Metamorphoses, Or Golden Ass, the God of Socrates, the Florida, and His Defence, Or a Discourse on Magic. READ BOOKS. 
  16. ↑ Manual of Mythology: for the use of schools, art students, and general readers founded on the works of Petiscus, Preller, and Welcker, Murray, A. S., Asher: 1873, Original from Oxford University, Digitized 19 Jan 2007
  17. ↑ Varro, De lingua Latina, v. 72, "Salacia Neptuni a salo."
  18. ↑ Augustine, De civitate Dei, vii. 22, "Jam utique habebat Salaciam Neptunus uxoreum"; Servicius, on Virgil, Aen, x. 76, "Sane hane Veniliam quidam Salaciam accipiunt, Neptuni uxorem."
  19. ↑ Adonis Attis Osiris: Studies in the History of Oriental Religion, Frazer, J. G., Edition: 3, Kessinger Publishing: 2003
  20. ↑ A Dictionary of Greek and Roman biography and mythology, Salacia
  21. ↑ "MPC/MPO/MPS Archive". Minor Planet Center. https://www.minorplanetcenter.net/iau/ECS/MPCArchive/MPCArchive_TBL.html. 
  22. ↑ Kerényi, Carl (1951). The Gods of the Greeks. London: Thames and Hudson. p. 64. 
  23. ↑ Homer, Iliad 18.41; Apollodorus, 1.2.7; Hesiod, Theogony 240
  24. ↑ Bane, Theresa (2013). Encyclopedia of Fairies in World Folklore and Mythology. McFarland, Incorporated, Publishers. p. 11, 12. ISBN 978-0-7864-7111-9. 
  25. ↑ Miller, Kirk (26 October 2021). "Unicode request for dwarf-planet symbols". https://www.unicode.org/L2/L2021/21224-dwarf-planet-syms.pdf. 
  26. ↑ Miller, Kirk (18 October 2024). "Preliminary presentation of constellation symbols". The Unicode Consortium. https://www.unicode.org/L2/L2024/24235-constellation-symbols.pdf. 
  27. ↑ Lykawka, Patryk Sofia; Tadashi, Mukai (July 2007). "Dynamical classification of trans-neptunian objects: Probing their origin, evolution, and interrelation". Icarus 189 (1): 213–232. doi:10.1016/j.icarus.2007.01.001. Bibcode: 2007Icar..189..213L. 
  28. ↑ 28.0 28.1 "Occultation by Salacia (2018-12-27)". Lucky Star Project. 2018-12-27. https://lesia.obspm.fr/lucky-star/single.php?p=3352. 
  29. ↑ 29.0 29.1 Attwood, Ben (July 2024). "Performing Automated, High-Speed Photometry on Occulting, Small Outer Solar System Objects". Edinburgh Student Journal of Science. https://www.medanthrotheory.org/esjs/article/download/9682/12433. 
  30. ↑ 30.0 30.1 30.2 30.3 Proudfoot, Benjamin; Parker, Alex H.; Grundy, William M.; Noll, Keith S.; Porter, Simon B. (July 19, 2024). "17848 - Astrometry for an Upcoming Double Occultation of Salacia-Actaea". Hubble Space Telescope Observation Programs. https://www.stsci.edu/hst-program-info/download/hst/pdf/17848/. 
  31. ↑ 31.0 31.1 31.2 "Occultation by Salacia (2024-08-17)". Lucky Star Project. 2024-08-17. https://lesia.obspm.fr/lucky-star/occ.php?p=131439. 
  32. ↑ 32.0 32.1 Buie, Marc W. (2027-01-26). "RECON Occultation Details for (120347) Salacia on 2027 January 26". https://www2.boulder.swri.edu/~buie/recon/events/120347_270126_2141514.html. 
  33. ↑ Buie, Marc W.; Keller, John M.; Nesvorný, David; Porter, Simon B. (January 2025). "Occultation constraints on solar system formation models". Philosophical Transactions of the Royal Society A: Mathematical, Physical and Engineering Sciences 383 (2291). doi:10.1098/rsta.2024.0194. https://royalsocietypublishing.org/rsta/article/383/2291/20240194/108397/Occultation-constraints-on-solar-system-formation. 
  34. ↑ 34.0 34.1 Camargo, J. I. B.; Vieira Martins, R.; Assafin, M.; Braga-Ribas, F.; Sicardy, B.; Gomes-Júnior, A. R.; Dias-Pinto, A. (January 2014). "Candidate stars for stellar occultations by Neptunian Trojans and TNOs up to 2015". Astronomy & Astrophysics 561: A37. doi:10.1051/0004-6361/201322584. http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/561/A37. 
  35. ↑ Santos-Sanz, P.; Ortiz, J. L.; Sicardy, B.. "Stellar Occultations by Trans-Neptunian Objects From Ground and Space". Gaya and TNOs Exploration Workshops. European Space Agency. https://www.cosmos.esa.int/documents/739790/758041/Santos-Sanz_modified.pdf/82dc16ea-0bf3-4314-a888-d46b67c4e710. 
  36. ↑ Thirouin, A.; Noll, K. S.; Ortiz, J. L.; Morales, N. (September 2014). "Rotational properties of the binary and non-binary populations in the Trans-Neptunian belt". Astronomy & Astrophysics 569: A3. doi:10.1051/0004-6361/201423567. Bibcode: 2014A&A...569A...3T. 
  37. ↑ J.A. Stansberry (2012). "Physical Properties of Trans-Neptunian Binaries (120347) Salacia–Actaea and (42355) Typhon–Echidna". Icarus (Elsevier) 219 (2): 676–688. doi:10.1016/j.icarus.2012.03.029. Bibcode: 2012Icar..219..676S. http://www.sciencedirect.com/science/article/pii/S0019103512001224. Retrieved 2012-04-27. 
  38. ↑ Fornasier, S. 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 & Astrophysics 555: A15. doi:10.1051/0004-6361/201321329. Bibcode: 2013A&A...555A..15F. https://www.aanda.org/articles/aa/full_html/2013/07/aa21329-13/aa21329-13.html. Retrieved 2026-05-06. 
  39. ↑ 39.0 39.1 Fornasier, S. et al. (2013). "TNOs are Cool: A survey of the trans-Neptunian region. VIII. Combined Herschel PACS and SPIRE observations of 9 bright targets at 70–500 μm". Astronomy & Astrophysics 555: A92. doi:10.1051/0004-6361/201321329. Bibcode: 2013A&A...555A..15F. 
  40. ↑ Brown, Michael E.; Butler, Bryan J. (22 January 2018). "Medium-sized satellites of large Kuiper belt objects". The Astronomical Journal 156 (4): 164. doi:10.3847/1538-3881/aad9f2. Bibcode: 2018AJ....156..164B. 
  41. ↑ 41.0 41.1 41.2 41.3 41.4 Grundy, W. M.; Noll, K. S.; Buie, M. W.; Benecchi, S. D.; Ragozzine, D.; Roe, H. G. (December 2019). "The Mutual Orbit, Mass, and Density of Transneptunian Binary Gǃkúnǁʼhòmdímà ((229762) 2007 UK126)". Icarus 334: 30–38. doi:10.1016/j.icarus.2018.12.037. Bibcode: 2019Icar..334...30G. http://www2.lowell.edu/users/grundy/abstracts/preprints/2019.G-G.pdf. 
  42. ↑ Brown, Michael E.; Butler, Bryan J. (1 October 2023). "Masses and Densities of Dwarf Planet Satellites Measured with ALMA". The Planetary Science Journal 4 (10): 193. doi:10.3847/PSJ/ace52a. Bibcode: 2023PSJ.....4..193B. 
  43. ↑ Brown, Michael E. (13 September 2019). "How many dwarf planets are there in the outer solar system?". California Institute of Technology. http://web.gps.caltech.edu/~mbrown/dps.html. 
  44. ↑ Schaller, E. L.; Brown, M. E. (2008). "Detection of Additional Members of the 2003 EL61 Collisional Family via Near-Infrared Spectroscopy". Astrophysical Journal 684 (2): L107–L109. doi:10.1086/592232. Bibcode: 2008ApJ...684L.107S. 
  45. ↑ "IAUC 8751: (120347) 2004 SB_60; 2006gi, 2006gj; V733 Cep". Cbat.eps.Harvard.edu. http://www.cbat.eps.harvard.edu/iauc/08700/08751.html. 
  46. ↑ Stern, S.A.; Bagenal, F.; Ennico, K.; Gladstone, G.R.; Grundy, W.M.; McKinnon, W.B.; Moore, J.M.; Olkin, C.B. et al. (October 16, 2015). "The Pluto system: Initial results from its exploration by New Horizons". Science 350 (6258). doi:10.1126/science.aad1815. PMID 26472913. Bibcode: 2015Sci...350.1815S. 
  47. ↑ Brown, Michael E.; Butler, Bryan J. (1 October 2023). "Masses and Densities of Dwarf Planet Satellites Measured with ALMA". The Planetary Science Journal 4 (10): 193. doi:10.3847/PSJ/ace52a. Bibcode: 2023PSJ.....4..193B. 
  48. ↑ Sickafoose, A. A.; Bosh, A. S.; Levine, S. E.; Zuluaga, C. A.; Genade, A.; Schindler, K.; Lister, T. A.; Person, M. J. (1 February 2019). "A stellar occultation by Vanth, a satellite of (90482) Orcus". Icarus 319: 657–668. doi:10.1016/j.icarus.2018.10.016. Bibcode: 2019Icar..319..657S. 
  49. ↑ 49.0 49.1 Zangari, Amanda M.; Finley, Tiffany J.; Stern, S. Alan; Tapley, Mark B. (May 2019). "Return to the Kuiper Belt: Launch Opportunities from 2025 to 2040". Journal of Spacecraft and Rockets 56 (3): 919–930. doi:10.2514/1.A34329. Bibcode: 2019JSpRo..56..919Z. 
  50. ↑ 50.0 50.1 Holler, Bryan; Bannister, Michele; Singer, Kelsi; Stern, S. Alan; Benecchi, Susan; Ore, Cristina (May 2021). "Prospects for Future Exploration of the Trans-Neptunian Region". Planetary Science and Astrobiology Decadal Survey 2023-2032. 53. Bulletin of the American Astronomical Society. doi:10.3847/25c2cfeb.5950ca1c. 228. Bibcode: 2021BAAS...53d.228H. https://hal.science/hal-03400878/document. 
  51. ↑ Walters, Samuel; Lyne, James E. (2020). "A Survey of Mission Opportunities to Trans-Neptunian Objects, Part VI: A Search for Multi-Target Missions". AIAA Propulsion and Energy 2020 Forum. doi:10.2514/6.2020-3831. https://www.researchgate.net/publication/344409907. 
  52. ↑ Lyne, James Evans; Gleaves, Ashley; Quigley, John; Yousef, Nicholas (August 2021). "A Survey of Mission Opportunities to Trans-Neptunian Objects - Part 7: Utilization of a Delta V Earth Gravity Assist". AAS/AIAA Astrodynamics Specialist Conference. https://www.researchgate.net/publication/355582324. 
  53. ↑ 53.0 53.1 Anderson, Canaan (August 2025). INVESTIGATION AND OPTIMIZING OF INTERPLANATARY TRAJECTORIES TO TRANS-NEPTUNIAN OBJECTS (Master's Thesis). University of Tennessee, Knoxville.
  54. ↑ Kreitzman Ethan Cansler, Jordan; Stewart, Charles W.; Cansler, Ethan; Brisby, Jake; Green, Matthew; Lyne, James Evans (2013). "Mission Opportunities to Trans-Neptunian Objects—Part III, Orbital Capture, Low-Thrust Trajectories and Vehicle Radiation Environment During Jovian Flyby". 2024 AAS/AIAA Astrodynamics Specialist Conference. Denver, Colorado. pp. 1487–1506. https://www.researchgate.net/publication/293081475. Retrieved 2025-10-19. 



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