65489 Ceto

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Ceto
65489 Ceto.tiff
Orbit (top view)
Discovery and designation
Discovered byC. A. Trujillo and M. Brown
Discovery sitePalomar
Discovery dateMarch 22, 2003
Designations
MPC designation65489
Named afterCeto
Alternative names2003 FX128
Minor planet categoryTNO
Centaur[1]
AdjectiveCetoean
Orbital characteristics[3]
Epoch 2455200.5 (2010-Jan-04.0)
Aphelion181.90 AU
Perihelion17.8125 AU
Semi-major axis99.86 AU
Eccentricity0.8216
Orbital period998 years
Mean anomaly7.384°
Inclination22.3229°
Longitude of ascending node172.0572°
Argument of perihelion319.594°
Known satellitesPhorcys
(132 +6
−14
 km in diameter)[2]
Physical characteristics
Dimensions281±11 km[4]
174 +16
−18
km[2]
Mass5.4 ± 0.4 ×1018 kg (system)[2]
Mean density1.37 g/cm3 (system)[2]
Equatorial surface gravity3.3 cm/s2[2]
Geometric albedo0.056±0.006[4]
0.084 ± 0.02[2]
Absolute magnitude (H)6.2[3]
 
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Ceto
65489 Ceto.tiff
Orbit (top view)
Discovery and designation
Discovered byC. A. Trujillo and M. Brown
Discovery sitePalomar
Discovery dateMarch 22, 2003
Designations
MPC designation65489
Named afterCeto
Alternative names2003 FX128
Minor planet categoryTNO
Centaur[1]
AdjectiveCetoean
Orbital characteristics[3]
Epoch 2455200.5 (2010-Jan-04.0)
Aphelion181.90 AU
Perihelion17.8125 AU
Semi-major axis99.86 AU
Eccentricity0.8216
Orbital period998 years
Mean anomaly7.384°
Inclination22.3229°
Longitude of ascending node172.0572°
Argument of perihelion319.594°
Known satellitesPhorcys
(132 +6
−14
 km in diameter)[2]
Physical characteristics
Dimensions281±11 km[4]
174 +16
−18
km[2]
Mass5.4 ± 0.4 ×1018 kg (system)[2]
Mean density1.37 g/cm3 (system)[2]
Equatorial surface gravity3.3 cm/s2[2]
Geometric albedo0.056±0.006[4]
0.084 ± 0.02[2]
Absolute magnitude (H)6.2[3]

65489 Ceto /ˈst/ 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 (/ˈfɔərsɨs/, formally (65849) Ceto I Phorcys), after the Greek sea god. The Ceto system is considered the second known binary centaur,[2] using an extended definition of a centaur as an object on an non-resonant (unstable) orbit with the perihelion inside the orbit of Neptune.[5] It came to perihelion in 1989.[3]

Physical characteristics[edit]

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.[2]

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.[2] Unless the bodies are porous, the density is consistent with rock–ice composition, with rock content around 50%.[2]

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.[2]

References[edit]

  1. ^ Marc W. Buie (2006-05-05). "Orbit Fit and Astrometric record for 65489". SwRI (Space Science Department). Retrieved 2009-01-25. 
  2. ^ 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. 
  3. ^ a b c "JPL Small-Body Database Browser: 65489 Ceto (2003 FX128)". 2006-05-05 last obs. Retrieved 2009-12-12. 
  4. ^ a b 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
  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, and 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. 

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