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Sinope (moon) - Simple English Wikipedia, the free encyclopedia

Sinope (moon)

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Sinope
Discovery
Discovered by: S. B. Nicholson
Discovery date: July 21, 1914
Orbital characteristics
Periapsis: 18,237,600 km
Apoapsis 30,191,200 km
Mean radius of orbit: 23,540,000 km[1]
Eccentricity: 0.25[1]
Orbital period: 724.1 d (1.95 a)[1]
Avg. orbital speed: 2.252 km/s
Inclination: 128.11° (to the ecliptic)
153.12° (to Jupiter's equator)[1]
Satellite of: Jupiter
Physical characteristics
Mean radius: ~19 km
Volume: ~28,700 km³
Mass: 7.5×1016 kg
Mean density: 2.6 g/cm³ (assumed)
Equatorial surface gravity: 0.014 m/s2 (0.001 g)
Escape velocity: ~0.023 km/s
Albedo: 0.04 (assumed)
Temperature: ~124 K

Sinope is a non-spherical moon of Jupiter. It was found by Seth Barnes Nicholson at Lick Observatory in 1914,[2] and is named after Sinope of Greek mythology.

Sinope did not get its present name until 1975[3][4]; before then, it was simply known as Jupiter IX. It was sometimes called "Hades"[5] between 1955 and 1975.

Sinope was the farthest known moon of Jupiter until the discovery of Megaclite in 2000. The farthest moon of Jupiter now known is S/2003 J 2.

Contents

[change] Orbit

Pasiphae group.
Pasiphae group.

Sinope orbits Jupiter on a high eccentricity and high inclination retrograde orbit. The orbital elements are as of January 2000.[1] They are changing a lot due to Solar and planetary perturbations. It is often believed to belong to the Pasiphaë group.[6] However, given its mean inclination and different colour, Sinope could be also an independent object, captured independently, unrelated to the collision and break-up at the origin of the group.[7] The diagram illustrates Sinope's orbital elements in relation to other moons of the group.

[change] Physical characteristics

Sinope has an estimated diameter of 38 km (assuming an albedo of 0.04)[6] The moon is red[7] unlike Pasiphae which is grey.

Its infrared spectrum is similar to D-type asteroids also different from Pasiphae.[8] These dissimilarities of the physical parameters suggest a different origin from the core members of the group.


[change] References

  1. 1.0 1.1 1.2 1.3 1.4 Jacobson, R. A. (2000). "The Orbits of the Outer Jovian Satellites". Astronomical Journal 120: pp. 2679-2686. DOI:10.1086/316817.
  2. Nicholson, S. B. (1914). "Discovery of the Ninth Satellite of Jupiter". Publications of the Astronomical Society of the Pacific 26: pp. 197-198.
  3. Nicholson, S. B. (April 1939). "The Satellites of Jupiter". Publications of the Astronomical Society of the Pacific 51 (300): pp. 85–94. (in which he declines to name the recently discovered satellites (pp. 93–94))
  4. IAUC 2846: Satellites of Jupiter 1974 October 7 (naming the moon)
  5. Payne-Gaposchkin, Cecilia; Katherine Haramundanis (1970). Introduction to Astronomy. Englewood Cliffs, N.J.: Prentice-Hall. ISBN 0-134-78107-4. 
  6. 6.0 6.1 Sheppard, S. S.; and Jewitt, D. C.; An Abundant Population of Small Irregular Satellites Around Jupiter, Nature, Vol. 423 (May 2003), pp. 261-263
  7. 7.0 7.1 Grav, T.; Holman, M. J.; Gladman, B. J.; and Aksnes, K.; Photometric Survey of the Irregular Satellites, Icarus, Vol. 166 (2003), pp. 33-45
  8. Grav, T., and Holman, M. J. (2004). "Near-Infrared Photometry of the Irregular Satellites of Jupiter and Saturn". The Astrophysical Journal 605: pp. L141–L144.

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