Sycorax (moon)
Discovery image of Sycorax
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Discovery[1]
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| Discovered by | using the Hale telescope |
| Discovery date | September 6, 1997 |
| Mean orbit radius | 12,179,000 km[2] |
| Eccentricity | 0.5224 |
| Orbital period | 1288.28 d |
| Inclination | 159° (to the ecliptic)[3] |
| Satellite of | Uranus |
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Physical characteristics
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| Mean radius | 75 km (estimate)[3][4] |
| Surface area | ~70,000 km² (estimate) |
| Volume | ~1,800,000 km³ (estimate) |
| Mass | ~2.3×1018 kg (estimate) |
| Mean density | ~1.3 g/cm³ (assumed) |
| Rotation period | 3.6 h[5] |
| Axial tilt | ? |
| Albedo | 0.04 (assumed)[3] |
| Temperature | ~65 K (estimate) |
| Apparent magnitude | 20.8 (V)[6] |
Sycorax (
/ˈsɪkəræks/ SIK-or-aks) is the largest retrograde irregular satellite of Uranus. Sycorax was discovered on 6 September 1997 by Brett J. Gladman, Philip D. Nicholson, Joseph A. Burns, and John J. Kavelaars using the 200-inch Hale telescope, together with Caliban, and given the temporary designation S/1997 U 2.[1]
Officially confirmed as Uranus XVII, it was named after Sycorax, Caliban's mother in William Shakespeare's play The Tempest.
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[edit] Orbit
Sycorax follows a distant orbit, more than 20 times further from Uranus than the furthest regular moon Oberon.[1] Its orbit is retrograde, moderately inclined and eccentric. The orbital parameters suggest that it may belong, together with Setebos and Prospero, to the same dynamic cluster, suggesting common origin.[7]
The diagram illustrates the orbital parameters of the retrograde irregular satellites of Uranus (in polar co-ordinates) with the eccentricity of the orbits represented by the segments extending from the pericentre to the apocentre.
[edit] Physical characteristics
The diameter of Sycorax is estimated at 150 km (assuming albedo of 0.04)[3][4] making it the largest irregular satellite of Uranus, comparable in size with Puck and with Himalia, the biggest irregular satellite of Jupiter.
The satellite appears light-red in the visible light (colour indices B–V = 0.87 V–R = 0.44,[8] B–V = 0.78 ± 0.02 V–R = 0.62 ± 0.01,[7] B–V = 0.839 ± 0.014 V–R = 0.531 ± 0.005[5]) redder than Himalia but still less red than most Kuiper belt objects. However in the near infrared the spectrum turns blue between 0.8 and 1.25 μm and finally becomes neutral at the longer wavelengths.[6]
The rotation period of Sycorax is estimated at about 3.6 hours. Rotation causes periodical variations of the visible magnitude with the amplitude of 0.07.[5]
[edit] Origin
Sycorax is hypothesized to be a captured object: it did not form in the accretionary disk, which existed around Uranus just after its formation. The exact capture mechanism is not known, but capturing a moon requires the dissipation of energy. The possible capture processes include: gas drag in the protoplanetary disk, many-body interactions and the capture during the fast growth of the Uranus' mass (so called pull-down).[3][5]
[edit] See also
[edit] References
- ^ a b c Gladman, Brett J.; Nicholson, Philip D.; Burns, Joseph A.; Kavelaars, JJ; Marsden, Brian G.; Williams, Gareth V.; Offutt, Warren B. (1998). "Discovery of two distant irregular moons of Uranus". Nature 392 (6679): 897–899. Bibcode 1998Natur.392..897G. doi:10.1038/31890.
- ^ Jacobson, R.A. (2003) URA067 (2007-06-28). "Planetary Satellite Mean Orbital Parameters". JPL/NASA. http://ssd.jpl.nasa.gov/?sat_elem#uranus. Retrieved 2008-01-23.
- ^ a b c d e Sheppard, Scott S.; Jewitt, David C.; Kleyna, Jan (2005). "An Ultradeep Survey for Irregular Satellites of Uranus: Limits to Completeness" (PDF). The Astronomical Journal 129 (1): 518–525. arXiv:astro-ph/0410059. Bibcode 2005AJ....129..518S. doi:10.1086/426329. http://www.ifa.hawaii.edu/~jewitt/papers/2005/SJK2005.pdf. Retrieved 20 October 2009. "Table 3 ... ri (km) ... 36 ... i Radius of satellite assuming a geometric albedo of 0.04."[dead link]
- ^ a b "Planetary Satellite Physical Parameters". JPL (Solar System Dynamics). 2008-12-20. http://ssd.jpl.nasa.gov/?sat_phys_par. Retrieved 2009-03-10.
- ^ a b c d Maris, M.; Garraro, G.; Parisi, M.G. (2007). "Light curves and colours of the faint Uranian irregular satellites Sycorax, Prospero, Stephano, Setebos, and Trinculo". Astronomy&Astrophysics 472 (1): 311–319. arXiv:0704.2187. Bibcode 2007A&A...472..311M. doi:10.1051/0004-6361:20066927.
- ^ a b Romon, J.; de Bergh, C. et al (2001). "Photometric and spectroscopic observations of Sycorax, satellite of Uranus". Astronomy&Astrophysics 376 (1): 310–315. Bibcode 2001A&A...376..310R. doi:10.1051/0004-6361:20010934.
- ^ a b Grav, Tommy; Holman, Matthew J.; Fraser, Wesley C. (2004-09-20). "Photometry of Irregular Satellites of Uranus and Neptune". The Astrophysical Journal 613 (1): L77–L80. arXiv:astro-ph/0405605. Bibcode 2004ApJ...613L..77G. doi:10.1086/424997.
- ^ Rettig, Terrence W.; Walsh, Kevin; Consolmagno, Guy (December 2001). "Implied Evolutionary Differences of the Jovian Irregular Satellites from a BVR Color Survey". Icarus 154 (2): 313–320. Bibcode 2001Icar..154..313R. doi:10.1006/icar.2001.6715.
[edit] External links
- Sycorax Profile (by NASA's Solar System Exploration)
- David Jewitt pages
- Uranus' Known Satellites (by Scott S. Sheppard)
- MPC: Natural Satellites Ephemeris Service
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