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Proteus (moon)

Topic: Astronomy

 From HandWiki - Reading time: 8 min
Short description: Large moon of Neptune
Proteus
Proteus (Voyager 2).jpg
Voyager 2 image (1989)
Discovery
Discovered byVoyager 2
Stephen P. Synnott
Discovery dateJune 16, 1989
Designations
Designation
Neptune VIII
Pronunciation/ˈproʊtiəs/ PROH-tee-əs[1]
Named afterProteus (Ancient Greek:)
S/1989 N 1
AdjectivesProtean (/ˈproʊtiən/ PROH-tee-ən or /proʊˈtiːən/ proh-TEE-ən)[2]
Orbital characteristics[3]
Epoch 18 August 1989
|{{{apsis}}}|apsis}}117584±10 km
|{{{apsis}}}|apsis}}117709±10 km
117647±1 km (4.75 RN)
Eccentricity0.00053±0.00009
Orbital period1.12231477±0.00000002 d
Average Orbital speed7.623 km/s
Inclination0.524° (to Neptune's equator)
0.026°±0.007° (to local Laplace plane)
Satellite ofNeptune
Physical characteristics
Dimensions424 × 390 × 396 km[4][lower-alpha 1]
Mean radius210±7 km[7]
Surface area554,200 km2[8]
Volume(3.4±0.4)×107 km3[4]
Mass4.4×1019 kg (7.3672×10−6 Earths)[lower-alpha 2]
Mean density≈ 1.3 g/cm3 (estimate)[7]
0.07 m/s2[lower-alpha 3]
0.17 km/s[lower-alpha 4]
Rotation periodsynchronous[4]
Axial tiltzero[4]
Albedo0.096[7][9]
Physics≈ 51 K mean (estimate)
Apparent magnitude19.7[7]


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 spacecraft in 1989, it is named after Proteus, the shape-changing sea god of Greek mythology.[10] 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.[11] 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.[12]

Discovery and naming

Hubble Space Telescope image of Neptune and 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 the third moon of Neptune to be discovered, 40 years after the discovery of Neptune's moon Nereid in 1949.[13]

Upon discovery, Proteus received the temporary provisional designation S/1989 N 1.[14] 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.[15]

On 16 September 1991, S/1989 N 1 was named after Proteus, the shape-changing sea god of Greek mythology.[10]

Orbit

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 makes one orbit for every two orbits made by Larissa. Due to the outward tidal migration of Proteus in the past, the orbital resonances of Proteus and Larissa are no longer in effect.[16] Proteus may have ceased its integral orbital resonance with Larissa several hundred million years ago.[16][17]

Physical characteristics

Colorized Voyager 2 image of Proteus, with its large crater Pharos located at the right

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.[14]

Composition

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.[14] 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. Although Proteus is usually thought to contain significant amounts of water ice, it has not been detected spectroscopically on the surface.[11]

Shape

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] Saturn's moon Mimas has an ellipsoidal shape despite being slightly less massive than Proteus, perhaps due to the higher temperature near Saturn or tidal heating.[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

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

Proteus is heavily cratered, showing no sign of any geological modification.[14] 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.[18] 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

Protean craters are named after water-related spirits, gods, goddesses (excluding Greek and Roman names). As of June 2021, there is only one named crater on this body.[18]

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

Origin

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.[12] Only after Triton's orbit became circularised did some of the rubble disc re-accrete into the present-day moons of Neptune.[19]

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.[20] 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.[20]

Notes

  1. ↑ In the earlier papers slightly different dimensions were reported. Thomas and Veverka in 1991 reported 440×416×404 km.[4][5] Croft in 1992 reported 430×424×410 km.[6] 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. ↑ The mass was calculated by multiplying the volume from Stooke (1994)[4] by the assumed density of 1,300 kg/m3. If one uses slightly larger dimensions from the earlier papers the mass will increase to 5×1019 kg.[7]
  3. ↑ Surface gravity derived from the mass m, the gravitational constant G and the radius r: Gm/r2.
  4. ↑ Escape velocity derived from the mass m, the gravitational constant G and the radius r: √2Gm/r.

References

  1. ↑ "Proteus". Proteus. Oxford University Press. http://www.lexico.com/definition/Proteus. 
  2. ↑ Protean (3rd ed.), Oxford University Press, September 2005, http://oed.com/search?searchType=dictionary&q=Protean  (Subscription or UK public library membership required.)
  3. ↑ 3.0 3.1 3.2 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. doi:10.1086/423037. Bibcode: 2004AJ....128.1412J. 
  4. ↑ 4.00 4.01 4.02 4.03 4.04 4.05 4.06 4.07 4.08 4.09 4.10 4.11 4.12 Stooke, Philip J. (1994). "The surfaces of Larissa and Proteus". Earth, Moon, and Planets 65 (1): 31–54. doi:10.1007/BF00572198. Bibcode: 1994EM&P...65...31S. 
  5. ↑ Williams, Dr. David R. (2008-01-22). "Neptunian Satellite Fact Sheet". NASA (National Space Science Data Center). http://nssdc.gsfc.nasa.gov/planetary/factsheet/neptuniansatfact.html. 
  6. ↑ 6.0 6.1 6.2 6.3 6.4 6.5 6.6 Croft, S. (1992). "Proteus: Geology, shape, and catastrophic destruction". Icarus 99 (2): 402–408. doi:10.1016/0019-1035(92)90156-2. Bibcode: 1992Icar...99..402C. 
  7. ↑ 7.0 7.1 7.2 7.3 7.4 "Planetary Satellite Physical Parameters". JPL (Solar System Dynamics). 2010-10-18. http://ssd.jpl.nasa.gov/?sat_phys_par. 
  8. ↑ "Proteus By The Numbers". https://solarsystem.nasa.gov/moons/neptune-moons/proteus/by-the-numbers/. 
  9. ↑ Karkoschka, Erich (2003). "Sizes, shapes, and albedos of the inner satellites of Neptune". Icarus 162 (2): 400–407. doi:10.1016/S0019-1035(03)00002-2. Bibcode: 2003Icar..162..400K. 
  10. ↑ 10.0 10.1 Marsden, Brian G. (September 16, 1991). "Satellites of Saturn and Neptune". IAU Circular 5347. http://www.cbat.eps.harvard.edu/iauc/05300/05347.html. Retrieved 2011-10-24. 
  11. ↑ 11.0 11.1 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. doi:10.1086/375909. Bibcode: 2003AJ....126.1080D. 
  12. ↑ 12.0 12.1 Goldreich, P.; Murray, N.; Longaretti, P. Y.; Banfield, D. (1989). "Neptune's story". Science 245 (4917): 500–504. doi:10.1126/science.245.4917.500. PMID 17750259. Bibcode: 1989Sci...245..500G. 
  13. ↑ "Proteus In Depth". NASA Solar System Exporation. https://solarsystem.nasa.gov/moons/neptune-moons/proteus/in-depth/. 
  14. ↑ 14.0 14.1 14.2 14.3 Smith, B. A.; Soderblom, L. A.; Banfield, D.; Barnet, C.; Basilevsky, A. T.; Beebe, R. F.; Bollinger, K.; Boyce, J. M. et al. (1989). "Voyager 2 at Neptune: Imaging Science Results". Science 246 (4936): 1422–1449. doi:10.1126/science.246.4936.1422. PMID 17755997. Bibcode: 1989Sci...246.1422S. https://zenodo.org/record/1230992. 
  15. ↑ Green, Daniel W. E. (July 7, 1989). "1989 N 1". IAU Circular 4806. http://www.cbat.eps.harvard.edu/iauc/04800/04806.html. Retrieved 2011-10-24. 
  16. ↑ 16.0 16.1 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. doi:10.1016/j.icarus.2006.12.002. Bibcode: 2007Icar..188..386Z. 
  17. ↑ 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. doi:10.1016/j.icarus.2007.08.024. Bibcode: 2008Icar..193..267Z. 
  18. ↑ 18.0 18.1 "Planetary Names: Crater, craters: Pharos on Proteus". Gazetteer of Planetary Nomenclature. USGS Astrogeology. https://planetarynames.wr.usgs.gov/Feature/4684?__fsk=-1708907535. 
  19. ↑ Banfield, Don; Murray, Norm (October 1992). "A dynamical history of the inner Neptunian satellites". Icarus 99 (2): 390–401. doi:10.1016/0019-1035(92)90155-Z. Bibcode: 1992Icar...99..390B. 
  20. ↑ 20.0 20.1 Showalter, M. R.; de Pater, I.; Lissauer, J. J.; French, R. S. (2019). "The seventh inner moon of Neptune". Nature 566 (7744): 350–353. doi:10.1038/s41586-019-0909-9. PMID 30787452. PMC 6424524. Bibcode: 2019Natur.566..350S. https://www.spacetelescope.org/static/archives/releases/science_papers/heic1904/heic1904a.pdf. 

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