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Proteus (moon)

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Proteus
Processed grayscale image of Proteus from Voyager 2, August 1989 (image processing date). The massive crater Pharos occupies much of the upper right, straddling Proteus's terminator
Discovery
Discovered byVoyager 2
Stephen P. Synnott
Discovery dateJune 16, 1989
Designations
Designation
Neptune VIII
Pronunciation/ˈproʊtiəs/ PROH-tee-əs[1]
Named after
Πρωτεύς or Πρωτέας, Prōteys or Prōteas
S/1989 N 1
AdjectivesProtean (/ˈproʊtiən/ PROH-tee-ən or /proʊˈtiːən/ proh-TEE-ən)[2]
Orbital characteristics[3]
Epoch 18 August 1989
Periapsis117584±10 km
Apoapsis117709±10 km
117647±1 km (4.75 RN)
Eccentricity0.00053±0.00009
1.12231477±0.00000002 d
7.623 km/s
Inclination0.524° (to Neptune's equator)
0.026°±0.007° (to local Laplace plane)
Satellite ofNeptune
Physical characteristics
Dimensions424 km × 390 km × 396 km[4]
[a]
209±8 km[6]
210±7 km[7]
554 200 km2[8]
Volume(3.4±0.4)×107 km3[4]
Mass≈ (1.55–3.10)×1019 kg[b]
≈ (2.60–5.20)×10−6 Earths
Mean density
≈ 0.46–0.91 g/cm3[9][c]
≈ 0.023–0.054 m/s2[d]
≈ 0.099–0.146 km/s[e]
synchronous[4]
zero[4]
Albedo0.096[10][7]
Temperature≈ 51 K mean (estimate)
19.7[10]

Proteus (/ˈproʊtiəs/ PROH-tee-əs), also known as Neptune VIII, is the second-largest Neptunian moon, and Neptune's largest inner satellite. Discovered by Voyager 2 in 1989, it is named after Proteus, the shape-changing sea god of Greek mythology.[11] Proteus orbits Neptune in a nearly equatorial orbit at a distance of about 4.75 times the radius of Neptune's equator.[3]

Despite being a predominantly icy body more than 400 km (250 mi) in diameter, Proteus's shape deviates significantly from an ellipsoid.[6] It is shaped more like an irregular polyhedron with several slightly concave facets and relief as high as 20 km (12 mi). Its surface is dark, neutral in color, and heavily cratered.[12] Proteus's largest crater is Pharos, which is more than 230 km (140 mi) in diameter. There are also a number of scarps, grooves, and valleys related to large craters.

Proteus is probably not an original body that formed with Neptune. It could have accreted later from the debris formed when the largest Neptunian satellite, Triton, was captured.[13]

Discovery and naming

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Voyager 2, the space probe that discovered Proteus

Proteus was discovered from the images taken by the Voyager 2 space probe two months before its Neptune flyby in August 1989. Proteus was discovered 40 years after the discovery of Neptune's moon Nereid in 1949.[14]

Upon discovery, Proteus received the temporary provisional designation S/1989 N 1.[15] Stephen P. Synnott and Bradford A. Smith announced its discovery on July 7, 1989, speaking only of "17 frames taken over 21 days", which gives a discovery date of sometime before June 16.[16]

On 16 September 1991, S/1989 N 1 was named after Proteus, the shape-changing sea god of Greek mythology[11] following the convention that moons of Neptune should be named after deities and creatures related to the sea.

Orbit

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Hubble Space Telescope image of Neptune and Proteus

Proteus orbits Neptune at a distance of approximately 117,647 km (73,102 mi), nearly equal to 4.75 times the equatorial radius of the planet. The orbit of Proteus is nearly circular, having a small orbital eccentricity, and is inclined by about 0.5 degrees to Neptune's equator.[3] Proteus is tidally locked to Neptune, and rotates synchronously with its orbital motion, which means that Proteus always presents the same face to Neptune.[4]

Proteus may have once been in a 1:2 orbital resonance with Larissa, where Proteus made one orbit for every two orbits made by Larissa. Due to the outward tidal migration of Proteus over time, this is no longer the case.[17] Proteus may have ceased its integral orbital resonance with Larissa several hundred million years ago.[17][9]

Physical characteristics

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Size comparison between Proteus (lower left), the Moon (upper left) and Earth

Proteus is the second-largest moon of Neptune and is the largest of its regular prograde moons. It is about 420 km (260 mi) in diameter, larger than Nereid, Neptune's third-largest moon. It was not discovered by Earth-based telescopes because Proteus orbits so close to Neptune that it is lost in the glare of reflected sunlight.[15]

Composition

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False-color Voyager 2 image of Proteus, with its large crater Pharos located at the right

The surface of Proteus is dark as it has a geometrical albedo of about 10 percent–meaning that its surface reflects 10 percent of the light it receives from the Sun. The color of its surface is neutral as the reflectivity does not change appreciably with the wavelength from violet to green.[15] In the near-infrared range of around the wavelength of 2 μm, Proteus's surface becomes less reflective, indicating the possible presence of complex organic compounds such as hydrocarbons or cyanides. These compounds may be responsible for the low albedo of the inner Neptunian moons. While Proteus is usually thought to contain significant amounts of water ice, there is no definite spectroscopic confirmation of its presence on the surface.[12] However, James Webb Space Telescope NIRCam spectrophotometry of the moon has revealed a 3 μm absorption feature, indicating possible water ice or hydrated minerals on the surface of Proteus.[18] Proteus's infrared albedo measured at 1.4, 2.1, 3.0, and 4.6 microns appears to match other dark Solar System small bodies, such as 2004 EW95.[18]

Shape

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The shape of Proteus is close to a sphere with a radius of about 210 km (130 mi), although deviations from the spherical shape are large—up to 20 km (12 mi); scientists believe it is about as large as a body of its density can be without being pulled into a perfect spherical shape by its own gravity.[6] Proteus is slightly elongated in the direction of Neptune, although its overall shape is closer to an irregular polyhedron than to a triaxial ellipsoid. The surface of Proteus shows several flat or slightly concave facets measuring from 150 to 200 km in diameter. They are probably degraded impact craters.[4]

Surface features

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Voyager 2 image of Proteus, digitally processed showing surface features
Map of Proteus

Proteus is heavily cratered, showing no sign of any geological modification.[15] The largest crater, Pharos, has a diameter from 230 to 260 km.[6] Its depth is about 10–15 km.[4] The crater has a central dome on its floor a few kilometres high.[4] Pharos is the only named surface feature on this moon: the name is Greek and refers to the island where Proteus reigned.[19] In addition to Pharos there are several craters 50–100 km in diameter and many more with diameters less than 50 km.[4]

Other landforms on Proteus include linear features such as scarps, valleys, and grooves. The most prominent one runs parallel to the equator to the west of Pharos. These features likely formed as a result of the giant impacts, which formed Pharos and other large craters or as a result of tidal stresses from Neptune.[4][6]

Named features

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Protean craters are named after water-related spirits, gods, goddesses (excluding Greek and Roman names). As of May 2024, there is only one named crater on this body.[19]

Crater Pronunciation Diameter Approval
Year		 Eponym Ref
Pharos /ˈfɛərɒs/ FAIR-oss 230–260 km[6] 1994 Lighthouse of Alexandria (Pharos), island where Proteus reigned WGPSN

Origin

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Proteus, like the other inner moons of Neptune, is unlikely to be an original body that formed with it, and is more likely to have accreted from the rubble that was produced after Triton's capture. Triton's orbit upon capture would have been highly eccentric, and would have caused chaotic perturbations in the orbits of the original inner Neptunian moons, causing them to collide and reduce to a disc of rubble.[13] Only after Triton's orbit became circularised did some of the rubble disc re-accrete into the present-day moons of Neptune.[20]

Proteus initially had a smaller orbit around Neptune, and may have formed closer to the planet. At the time of the formation of Proteus, its orbit was estimated to be 8,000 km (5,000 mi) less than its current distance from Neptune.[21] Over time, Proteus migrated outward from Neptune through tidal interactions. During the outward migration of Proteus, collisions and impact events may have formed large craters and had ejected fragments of Proteus into orbit around Neptune. A collision of Proteus and another object could possibly explain the origin of Neptune's smaller moon Hippocamp, which orbits close to Proteus.[21]

Notes

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  1. ^ In other papers slightly different dimensions were reported. Thomas and Veverka in 1991 reported 440 km × 416 km × 404 km.[4][5] Croft in 1992 reported 430 km × 424 km × 410 km.[6] Karkoschka in 2003 reported (440±12) × (416±16) × (404±20) km.[7] The difference is caused by the use of different sets of images and by the fact that the shape of Proteus is not described well by a triaxial ellipsoid.[4]
  2. ^ A density of 0.4–0.8 g/cm3 was calculated by approximating the volume as a sphere with a radius of 210±7 km.[9] The mass was calculated with the provided density and the assumed volume.
  3. ^ Density obtained from the calculated mass and the provided volume of (3.4±0.4)×107 km3 from Stooke (1994).[4]
  4. ^ Surface gravity derived from the mass m, the gravitational constant G and the radius r:
  5. ^ Escape velocity derived from the mass m, the gravitational constant G and the radius r:

References

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  1. ^ "Proteus". Lexico UK English Dictionary. Oxford University Press. Archived from the original on March 22, 2020.
  2. ^ "Protean". Oxford English Dictionary (Online ed.). Oxford University Press. (Subscription or participating institution membership required.)
  3. ^ a b c Jacobson, R. A.; Owen, W. M. Jr. (2004). "The orbits of the inner Neptunian satellites from Voyager, Earthbased, and Hubble Space Telescope observations". Astronomical Journal. 128 (3): 1412–1417. Bibcode:2004AJ....128.1412J. doi:10.1086/423037.
  4. ^ a b c d e f g h i j k l m Stooke, Philip J. (1994). "The surfaces of Larissa and Proteus". Earth, Moon, and Planets. 65 (1): 31–54. Bibcode:1994EM&P...65...31S. doi:10.1007/BF00572198. S2CID 121825800.
  5. ^ Williams, Dr. David R. (2008-01-22). "Neptunian Satellite Fact Sheet". NASA (National Space Science Data Center). Retrieved 2008-12-12.
  6. ^ a b c d e f g Croft, S. (1992). "Proteus: Geology, shape, and catastrophic destruction". Icarus. 99 (2): 402–408. Bibcode:1992Icar...99..402C. doi:10.1016/0019-1035(92)90156-2.
  7. ^ a b c Karkoschka, Erich (2003). "Sizes, shapes, and albedos of the inner satellites of Neptune". Icarus. 162 (2): 400–407. Bibcode:2003Icar..162..400K. doi:10.1016/S0019-1035(03)00002-2.
  8. ^ "Proteus By The Numbers". solarsystem.nasa.gov/. Retrieved September 4, 2020.
  9. ^ a b c Zhang, K.; Hamilton, D. P. (2008). "Orbital resonances in the inner Neptunian system: II. Resonant history of Proteus, Larissa, Galatea, and Despina". Icarus. 193 (1): 267–282. Bibcode:2008Icar..193..267Z. doi:10.1016/j.icarus.2007.08.024.
  10. ^ a b "Planetary Satellite Physical Parameters". JPL (Solar System Dynamics). 2010-10-18. Retrieved 2011-10-11.
  11. ^ a b Marsden, Brian G. (September 16, 1991). "Satellites of Saturn and Neptune". IAU Circular. 5347. Retrieved 2011-10-24.
  12. ^ a b Dumas, Christophe; Smith, Bradford A.; Terrile, Richard J. (2003). "Hubble Space Telescope NICMOS Multiband Photometry of Proteus and Puck". The Astronomical Journal. 126 (2): 1080–1085. Bibcode:2003AJ....126.1080D. doi:10.1086/375909.
  13. ^ a b Goldreich, P.; Murray, N.; Longaretti, P. Y.; Banfield, D. (1989). "Neptune's story". Science. 245 (4917): 500–504. Bibcode:1989Sci...245..500G. doi:10.1126/science.245.4917.500. PMID 17750259. S2CID 34095237.
  14. ^ "Proteus In Depth". NASA Solar System Exporation. Archived from the original on 2023-09-21. Retrieved 12 March 2019.
  15. ^ a b c d Smith, B. A.; Soderblom, L. A.; Banfield, D.; Barnet, C.; Basilevsky, A. T.; Beebe, R. F.; Bollinger, K.; Boyce, J. M.; Brahic, A. (1989). "Voyager 2 at Neptune: Imaging Science Results". Science. 246 (4936): 1422–1449. Bibcode:1989Sci...246.1422S. doi:10.1126/science.246.4936.1422. PMID 17755997. S2CID 45403579.
  16. ^ Green, Daniel W. E. (July 7, 1989). "1989 N 1". IAU Circular. 4806. Retrieved 2011-10-24.
  17. ^ a b Zhang, K.; Hamilton, D. P. (2007). "Orbital resonances in the inner Neptunian system: I. The 2:1 Proteus–Larissa mean-motion resonance". Icarus. 188 (2): 386–399. Bibcode:2007Icar..188..386Z. doi:10.1016/j.icarus.2006.12.002.
  18. ^ a b Belyakov, Matthew; Davis, M. Ryleigh; Milby, Zachariah; Wong, Ian; Brown, Michael E. (2024-05-01). "JWST Spectrophotometry of the Small Satellites of Uranus and Neptune". The Planetary Science Journal. 5 (5): 119. arXiv:2404.06660. Bibcode:2024PSJ.....5..119B. doi:10.3847/PSJ/ad3d55. ISSN 2632-3338.
  19. ^ a b "Planetary Names: Crater, craters: Pharos on Proteus". Gazetteer of Planetary Nomenclature. USGS Astrogeology. Retrieved 24 June 2021.
  20. ^ Banfield, Don; Murray, Norm (October 1992). "A dynamical history of the inner Neptunian satellites". Icarus. 99 (2): 390–401. Bibcode:1992Icar...99..390B. doi:10.1016/0019-1035(92)90155-Z.
  21. ^ a b Showalter, M. R.; de Pater, I.; Lissauer, J. J.; French, R. S. (2019). "The seventh inner moon of Neptune" (PDF). Nature. 566 (7744): 350–353. Bibcode:2019Natur.566..350S. doi:10.1038/s41586-019-0909-9. PMC 6424524. PMID 30787452.
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