Proteus (moon)

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There is also an asteroid called 9313 Protea.
Proteus
Discovery
Discovered by: Voyager 2
Stephen P. Synnott
Discovery date: ~June 16, 1989
Orbital characteristics [1]
Epoch 18 August 1989
Periapsis: 117,584 ± 10 km
Apoapsis 117,709 ± 10 km
Semi-major axis: 117,647 ± 1 km (0.00079 AU)
Eccentricity: 0.00053 ± 0.00009
Orbital period: 1.12231477 ± 0.00000002 d
Avg. orbital speed: 7.623 km/s
Inclination: 0.524° (to Neptune equator)
0.026 ± 0.007° (to local Laplace plane)
Satellite of: Neptune
Physical characteristics
Dimensions: 440×416×404 km (± ~15 km)[2]
Volume: 3.4 ± 0.3 ×107km³[3]
Mass: ~4.4×1019 kg (estimate)
Mean density: ~1.3 g/cm³ (estimate)
Equatorial surface gravity: ~0.06 m/s2 (0.006 g)
Escape velocity: ~0.16 km/s
Rotation period: synchronous
Axial tilt: zero
Albedo: 0.096[2]
Temperature: ~51 K mean (estimate)
Apparent magnitude: 20.3 [4]

Proteus (pronounced /ˈproʊtiəs/, Greek Πρωτεύς), or Neptune VIII, is the second largest Neptunian moon, and its largest inner satellite. It is named after Proteus, the shape-changing sea god of Greek mythology.

Contents

Proteus was discovered from the images taken by Voyager 2 probe during the Neptune flyby in 1989. It received the temporary designation S/1989 N 1. Stephen P. Synnott and Bradford A. Smith announced (IAUC 4806) 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. The name was given on 16 September 1991.[5]

Map of Proteus
Map of Proteus

Proteus is more than 400 kilometres in diameter, larger than Nereid, another moon of Neptune. However, it was not discovered by Earth-based telescopes because it is so close to the planet that it is lost in the glare of reflected sunlight.

Proteus is one of the darkest objects in the solar system, as dark as soot; like Saturn's moon Phoebe, it reflects only 6 percent of the sunlight that strikes it. Proteus is very cratered, showing no sign of any geological modification. It is also irregularly shaped; scientists believe Proteus is about as large as a body of its density can be without being pulled into a spherical shape by its own gravity. Saturn's moon Mimas has much more regular shape despite being less massive than Proteus.

A simulated view of Proteus orbiting Neptune
A simulated view of Proteus orbiting Neptune


  1. ^ R.A. Jacobson and W.M. Owen Jr. (2004). "The orbits of the inner Neptunian satellites from Voyager, Earthbased, and Hubble Space Telescope observations". Astronomical Journal 128: 1412. 
  2. ^ a b E. Karkoschka (2003). "Sizes, shapes, and albedos of the inner satellites of Neptune". Icarus 162: 400. 
  3. ^ P.J. Stooke (1994). "The surfaces of Larissa and Proteus". Earth, Moon ad Planets 65: 31. 
  4. ^ Proteus Statistics. Retrieved on 2007-10-01.
  5. ^ IAU Circular No. 5347 (September 16 1991). Retrieved on 2007-04-10.

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