65489 Ceto

Ceto
	Orbit (top view)
Discovery
Discovered by	C. A. Trujillo and M. Brown
Discovery site	Palomar
Discovery date	22 March 2003
Designations
MPC designation	(65489) Ceto
Named after	Ceto
Alternative designations	2003 FX128
Minor planet category	TNO; Centaur–extended
Adjectives	Cetoean
Orbital characteristics
	Epoch 13 January 2016 (JD 2457400.5)
	Uncertainty parameter 2
Observation arc	9239 days (25.30 yr)
Aphelion	187.74 AU (28.086 Tm)
Perihelion	17.8498 AU (2.67029 Tm)
Semi-major axis	102.79 AU (15.377 Tm)
Eccentricity	0.82635
Orbital period (sidereal)	1042.22 yr (380669.7 d)
Mean anomaly	9.1219°
Mean motion	0.00094570°/day
Inclination	22.266°
Longitude of ascending node	171.85°
Argument of perihelion	320.086°
Known satellites	Phorcys; (171±10 ~ 132+6; −14 km in diameter)
Earth MOID	16.895 AU (2.5275 Tm)
Jupiter MOID	12.7433 AU (1.90637 Tm)
Physical characteristics
Dimensions	223±10 km; 174+16; −18 km
Mass	(5.4±0.4)×1018 kg (system)
Mean density	1.37 g/cm3 (system)
Equatorial surface gravity	3.3 cm/s2
Synodic rotation period	4.43 h (0.185 d)
Geometric albedo	0.056±0.006; 0.084±0.02
Absolute magnitude (H)	6.54±0.06, 6.4

65489 Ceto /ˈsiːtoʊ/ is a binary trans-Neptunian object (TNO) discovered on March 22, 2003 by C. A. Trujillo and M. Brown at Palomar. It is named after the sea goddess Ceto from Greek mythology. The object was identified as a binary on April 11, 2006 by K. Noll, H. Levison, W. Grundy and D. Stephens using the Hubble Space Telescope; the companion object is named Phorcys (/ˈfɔːrsɪs/, formally (65849) Ceto I Phorcys), after the Greek sea god. Using an extended definition of a centaur as an object on a non-resonant (unstable) orbit with its perihelion inside the orbit of Neptune,^[5] the Ceto system can be considered the second known binary centaur.^[4] It came to perihelion in 1989.^[2]

Physical characteristics

65489 Ceto is an example of a close binary TNO system in which the components are of similar size. Combined observations with the infrared Spitzer Space Telescope and the Hubble Telescope allow the diameter of Ceto itself to be estimated at 174+16
−18 km and the diameter of Phorcys at 132+6
−14 km, assuming equal albedo for both components.^[4]

The binary nature of Ceto enables direct calculation of the system mass, allowing estimation of the masses of the components and providing additional constraints on their composition. The estimated density of Ceto is 1.37+0.66
−0.32 g/cm³, significantly less than that of the large TNOs (Haumea: 3.0 g/cm³, Eris: 2.26, Pluto: 2.03, Charon: 1.65) but significantly more than that of smaller TNOs (e.g. 0.7 g/cm³ for (26308) 1998 SM165). Phorcys has a mass of about 1.67×10¹⁸ kg.^[4] Unless the bodies are porous, the density is consistent with rock–ice composition, with rock content around 50%.^[4]

It has been suggested that tidal forces, together with other potential heat sources (e.g. collisions or ²⁶Al decay) might have raised the temperature sufficiently to crystallise amorphous ice and reduce the void space inside the object. The same tidal forces could be responsible for the quasi-circular orbits of the components of Ceto.^[4]

Ceto is listed on Michael Brown's website as possibly a dwarf planet.^[6]

References

^ Marc W. Buie (2006-05-05). "Orbit Fit and Astrometric record for 65489". SwRI (Space Science Department). Retrieved 2009-01-25.
^ ^a ^b ^c "JPL Small-Body Database Browser: 65489 Ceto (2003 FX128)" (2006-05-05 last obs). Retrieved 25 March 2016.
^ ^a ^b ^c ^d Santos-Sanz, P., Lellouch, E., Fornasier, S., Kiss, C., Pal, A., Müller, T. G., Vilenius, E., Stansberry, J., Mommert, M., Delsanti, A., Mueller, M., Peixinho, N., Henry, F., Ortiz, J. L., Thirouin, A., Protopapa, S., Duffard, R., Szalai, N., Lim, T., Ejeta, C., Hartogh, P., Harris, A. W., & Rengel, M. (2012). “TNOs are Cool”: A Survey of the Transneptunian Region IV - Size/albedo characterization of 15 scattered disk and detached objects observed with Herschel Space Observatory-PACS
^ ^a ^b ^c ^d ^e ^f ^g ^h ⁱ ^j ^k Grundy, W.M.; Stansberry, J.A.; Noll K.S.; Stephens, D.C.; et al. (2007). "The orbit, mass, size, albedo, and density of (65489) Ceto/Phorcys: A tidally-evolved binary Centaur". Icarus. 191: 286. arXiv:0704.1523. Bibcode:2007Icar..191..286G. doi:10.1016/j.icarus.2007.04.004.
^ J. L. Elliot; S. D. Kern; K. B. Clancy; A. A. S. Gulbis; R. L. Millis; M. W. Buie; L. H. Wasserman; E. I. Chiang; A. B. Jordan; D. E. Trilling; K. J. Meech (February 2005). "The Deep Ecliptic Survey: A Search for Kuiper Belt Objects and Centaurs. II. Dynamical Classification, the Kuiper Belt Plane, and the Core Population" (PDF). The Astronomical Journal. 129: 1117. Bibcode:2005AJ....129.1117E. doi:10.1086/427395. {{cite journal}}: Unknown parameter |last-author-amp= ignored (|name-list-style= suggested) (help)
^ Michael E. Brown. "How many dwarf planets are there in the outer solar system? (updates daily)". California Institute of Technology. Archived from the original on 2011-10-18. Retrieved 2015-10-03. {{cite web}}: Unknown parameter |deadurl= ignored (|url-status= suggested) (help)

External links

Binary asteroids at johnstonsarchive
65489 Ceto at the JPL Small-Body Database
- Close approach · Discovery · Ephemeris · Orbit viewer · Orbit parameters · Physical parameters

[Buie-1] Marc W. Buie (2006-05-05). "Orbit Fit and Astrometric record for 65489". SwRI (Space Science Department). Retrieved 2009-01-25.

[jpldata-2] "JPL Small-Body Database Browser: 65489 Ceto (2003 FX128)" (2006-05-05 last obs). Retrieved 25 March 2016.

[TNOsCool4-3] Santos-Sanz, P., Lellouch, E., Fornasier, S., Kiss, C., Pal, A., Müller, T. G., Vilenius, E., Stansberry, J., Mommert, M., Delsanti, A., Mueller, M., Peixinho, N., Henry, F., Ortiz, J. L., Thirouin, A., Protopapa, S., Duffard, R., Szalai, N., Lim, T., Ejeta, C., Hartogh, P., Harris, A. W., & Rengel, M. (2012). “TNOs are Cool”: A Survey of the Transneptunian Region IV - Size/albedo characterization of 15 scattered disk and detached objects observed with Herschel Space Observatory-PACS

[Grundy2007-4] ^ ^a ^b ^c ^d ^e ^f ^g ^h ⁱ ^j ^k Grundy, W.M.; Stansberry, J.A.; Noll K.S.; Stephens, D.C.; et al. (2007). "The orbit, mass, size, albedo, and density of (65489) Ceto/Phorcys: A tidally-evolved binary Centaur". Icarus. 191: 286. arXiv:0704.1523. Bibcode:2007Icar..191..286G. doi:10.1016/j.icarus.2007.04.004.

[DES_Elliot2005-5] J. L. Elliot; S. D. Kern; K. B. Clancy; A. A. S. Gulbis; R. L. Millis; M. W. Buie; L. H. Wasserman; E. I. Chiang; A. B. Jordan; D. E. Trilling; K. J. Meech (February 2005). "The Deep Ecliptic Survey: A Search for Kuiper Belt Objects and Centaurs. II. Dynamical Classification, the Kuiper Belt Plane, and the Core Population" (PDF). The Astronomical Journal. 129: 1117. Bibcode:2005AJ....129.1117E. doi:10.1086/427395. {{cite journal}}: Unknown parameter |last-author-amp= ignored (|name-list-style= suggested) (help)

[Brown-dplist-6] Michael E. Brown. "How many dwarf planets are there in the outer solar system? (updates daily)". California Institute of Technology. Archived from the original on 2011-10-18. Retrieved 2015-10-03. {{cite web}}: Unknown parameter |deadurl= ignored (|url-status= suggested) (help)

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Physical characteristics

See also

References

External links