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Phoebe (moon)

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Phoebe
Discovery
Discovered byW.H. Pickering
Discovery date17 March 1899 / 16 August 1898
Designations
Saturn IX
AdjectivesPhoebean
Orbital characteristics[1]
12 955 759 km
Eccentricity0.156 241 5
550.564 636 d
Inclination173.04° (to the ecliptic)
151.78° (to Saturn's equator)
Satellite ofSaturn
Physical characteristics
Dimensions230 x 220 x 210 km
106.60 ± 1.00 km[1]
Mass(0.829 2 ± 0.001 0)×1019 kg [2]
Mean density
1.634 2 ± 0.046 0 g/cm³[1][2]
~0.049 m/s2
~0.10 km/s
0.386 75 d (9 h 16 min 55.2 s) [3]
152.14° [4]
Albedo0.06

Phoebe (Template:Pron-en,[5] or as Greek Φοίβη) is an irregular satellite of Saturn. It was discovered by William Henry Pickering on 17 March 1899 from photographic plates that had been taken starting on 16 August 1898 at Arequipa, Peru by DeLisle Stewart[6][7][8][9][10]. It was the first satellite to be discovered photographically.

Phoebe was the first target encountered upon the arrival of Cassini–Huygens to the Saturn system in 2004, and is thus unusually well-studied for a natural satellite of its size. Cassini's trajectory to Saturn and time of arrival were specifically chosen to permit this flyby.[11] After the encounter and its insertion orbit, Cassini would not go much beyond the orbit of Iapetus.

Name

The moon is named after Phoebe[8], a Titan in Greek mythology. It is also designated Saturn IX. The IAU nomenclature standards have stated that features on Phoebe are to be named after characters in the Greek myth of Jason and the Argonauts. In 2005, the IAU officially named 24 craters[12] (Acastus, Admetus, Amphion, Butes, Calais, Canthus, Clytius, Erginus, Euphemus, Eurydamas, Eurytion, Eurytus, Hylas, Idmon, Iphitus, Jason, Mopsus, Nauplius, Oileus, Peleus, Phlias, Talaus, Telamon, and Zetes).

Dr. Toby Owen of the University of Hawaii at Manoa, chairman of the International Astronomical Union Outer Solar System Task Group said

"We picked the legend of the Argonauts for Phoebe as it has some resonance with the exploration of the Saturn system by Cassini-Huygens. We can't say that our participating scientists include heroes like Hercules and Atalanta, but they do represent a wide, international spectrum of outstanding people who were willing to take the risk of joining this voyage to a distant realm in hopes of bringing back a grand prize."

Orbital characteristics

For more than 100 years, Phoebe was Saturn's outermost known moon, until the discovery of several smaller moons in 2000. Phoebe is almost 4 times more distant from Saturn than its nearest major neighbor (Iapetus), and is substantially larger than any of the other moons orbiting planets at comparable distances.

All of Saturn's moons up to Iapetus orbit very nearly in the plane of Saturn's equator. The outer irregular satellites follow fairly to highly eccentric orbits, and none is expected to rotate synchronously as all the inner moons of Saturn do (except for Hyperion). See Saturn's satellites families.

Physical characteristics

Closeup image of Phoebe from the Cassini-Huygens spacecraft, 13 June 2004.
Named craters on Phoebe.

Phoebe is roughly spherical and has a diameter of 220 kilometres (140 mi), which is equal to about one-fifteenth of the diameter of Earth's moon. Phoebe rotates on its axis every nine hours and it completes a full orbit around Saturn in about 18 months. Its surface temperature is 75 K (-198°C).

Most of Saturn's inner moons have very bright surfaces, but Phoebe's albedo is very low (0.06), as dark as lampblack. The Phoebean surface is extremely heavily scarred, with craters up to 80 kilometres across, one of which has walls 16 kilometres high.

Phoebe's dark coloring initially led to scientists surmising that it was a captured asteroid, as it resembled the common class of dark carbonaceous asteroids. These are chemically very primitive and are thought to be composed of original solids that condensed out of the solar nebula with little modification since then.

However, images from the Cassini-Huygens space probe indicate that Phoebe's craters show a considerable variation in brightness, which indicate the presence of large quantities of ice below a relatively thin blanket of dark surface deposits some 300 to 500 metres (980 to 1,640 ft) thick. In addition, quantities of carbon dioxide have been detected on the surface, a finding which has never been replicated on an asteroid. It is estimated that Phoebe is about 50% rock, as opposed to the 35% or so that typifies Saturn's inner moons. For these reasons, scientists are coming to believe that Phoebe is in fact a captured Centaur, one of a number of icy planetoids from the Kuiper belt that orbit the Sun between Jupiter and Neptune[13][14]. Phoebe is the first such object to be imaged as anything other than a dot.

Material displaced from Phoebe's surface by microscopic meteor impacts may be responsible for the dark surfaces of Hyperion[15]. Debris from the biggest impacts may have been the building blocks of the other moons of Phoebe's group—all of which are less than 10 km in diameter.

Map

A composite image of Phoebe's surface (143 kB). The higher latitudes have been clipped from the main map, but can be seen in the polar projection below.
The higher latitudes can be seen in this image.

Spacecraft flybys

Closeup image of Phoebe from Cassini-Huygens

The Voyager 2 spacecraft passed by Phoebe in September 1981, although the 2.2 Gm (2.2 million kilometres) distance and low resolution meant that relatively little could be learned from the resulting images.

The Cassini spacecraft flew within 2,068 kilometres (1,285 mi) of Phoebe on 11 June 2004, returning many high-resolution images of the moon and its scarred surface. By a stroke of pure luck, Phoebe happened to be in the best part of its orbit to be photographed by the incoming Cassini probe, which otherwise would not likely have returned pictures much better than Voyager due to Phoebe's distance from Saturn. In addition, due to its rapid rotation period of approximately 9 hours, 56 minutes, Cassini was able to map virtually the entire surface of Phoebe.

Phoebe ring

Main article: Rings of Saturn § Phoebe ring
Artists impression of the Phoebe ring which dwarfs the main rings.
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The Phoebe ring is one of the rings of Saturn. This ring is tilted 27 degrees from Saturn's equatorial plane (and the other rings). It extends from at least 128 to 207[16] times the radius of Saturn; Phoebe orbits the planet at an average distance of 215 Saturn radii. The ring is about 20 times as thick as the diameter of the planet.[17] Since the ring's particles are presumed to have originated from micrometeoroid impacts on Phoebe, they should share its retrograde orbit,[18] which is opposite to the orbital motion of the next inner moon, Iapetus. Inwardly migrating ring material would thus strike the Iapetus's leading hemisphere, possibly causing the two-tone coloration of that moon.[19] Although very large, the ring is virtually invisible—it was discovered using NASA's infra-red Spitzer Space Telescope.

See also

References

  1. ^ a b "Planetary Satellite Physical Parameters". JPL (Solar System Dynamics). 2008-10-24. Retrieved 2008-12-07.
  2. ^ a b Jacobson, R. A. (2006). "The Gravity Field of the Saturnian System from Satellite Observations and Spacecraft Tracking Data". The Astronomical Journal. 132: 2520–2526. doi:10.1086/508812. {{cite journal}}: Unknown parameter |coauthors= ignored (|author= suggested) (help); Unknown parameter |month= ignored (help)
  3. ^ Seidelmann, P. K.; Abalakin, V. K.; Bursa, M.; Davies, M. E.; de Bergh, C.; Lieske, J. H.; Oberst, J.; Simon, J. L.; Standish, E. M.; Stooke, P.; and Thomas, P. C.Report of the IAU/IAG Working Group on Cartographic Coordinates and Rotational Elements of the Planets and Satellites: 2000
  4. ^ Porco CC; et al. (2005-02-25). "Cassini Imaging Science: Initial Results on Phoebe and Iapetus". Science. 307 (5713): 1237–1242. doi:10.1126/science.1107981. {{cite journal}}: Explicit use of et al. in: |author= (help)CS1 maint: extra punctuation (link)
  5. ^ In US dictionary transcription, Template:USdict.
  6. ^ Pickering EC (1899-03-17). "A New Satellite of Saturn". 49. Harvard College Observatory Bulletin.
  7. ^ Pickering EC (1899-03-23). "A New Satellite of Saturn". Astronomical Journal. 20 (458): 13.
  8. ^ a b Pickering EC (1899-04-10). "A New Satellite of Saturn". Astrophysical Journal. 9 (4): 274–276.
  9. ^ Pickering EC (1899-04-29). "A New Satellite of Saturn". Astronomische Nachrichten. 149 (10): 189–192. (same as above)
  10. ^ "A Ninth Satellite to Saturn". The Observatory. 22 (278): 158–159. 1899. {{cite journal}}: Unknown parameter |month= ignored (help)
  11. ^ Martinez, Carolina (2004-06-09). "Cassini Spacecraft Near First Stop in Historic Saturn Tour". Mission News. NASA. Retrieved 2008-03-02. {{cite web}}: Unknown parameter |coauthors= ignored (|author= suggested) (help)
  12. ^ Features on Saturn's moon Phoebe given names, Spaceflight Now, February 24, 2005
  13. ^ Johnson, Torrence V.; and Lunine, Jonathan I.; Saturn's moon Phoebe as a captured body from the outer Solar System, Nature, Vol. 435, pp. 69–71
  14. ^ Martinez, C.; Scientists Discover Pluto Kin Is a Member of Saturn Family, Cassini-Huygens News Releases, May 6, 2005
  15. ^ The composition implied by spectra does not seem to support the earlier suggestion that Phoebe could be the source of the dark material deposited on Iapetus
  16. ^ Verbiscer, Anne (published online 2009-10-07). "Saturn's largest ring" (PDF). Nature. {{cite journal}}: Check date values in: |date= (help); Unknown parameter |coauthors= ignored (|author= suggested) (help)
  17. ^ "The King of Rings". NASA, Spitzer Space Telescope center. 2009-10-07. Retrieved October 7, 2009.
  18. ^ Cowen, Rob (October 6, 2009). "Largest known planetary ring discovered". Science News.
  19. ^ Largest ring in solar system found around Saturn, New Scientist

External links

Wikimedia Commons has media related to Phoebe.


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