Ceres (dwarf planet)
|Discovery and designation|
|Discovered by||Giuseppe Piazzi|
|Discovery date||January 1, 1801|
|Other names||A899 OF; 1943 XB|
Reference date November 26, 2005|
|Longest distance from the Sun||
|Shortest distance from the Sun||
|Longest distance from the center of its orbital path|
2.765 956 424 AU
|How long it takes to complete an orbit||
|Average speed||17.882 km/s|
|Angle above the reference plane|
|Size and other qualities|
|Average radius||473 km|
|Mass||9.46 ± 0.04×1020 kg|
|Average density||2.08 g/cm3|
|Escape velocity||0.51 km/s|
|How much light it reflects||0.113 (geometric)|
|6.7 to 9.32|
It was discovered on 1 January 1801, by Giuseppe Piazzi, and is named after the Roman goddess Ceres—the goddess of growing plants, the harvest, and of motherly love. After about 200 years from its discovery, the International Astronomical Union decided to upgrade Ceres from an asteroid (or minor planet) to dwarf planetary status in 2006.
With a diameter of about 950 km, Ceres is by far the largest and most massive object in the asteroid belt, and has about a third of the belt's total mass. It was once thought to be smaller than Vesta, which is brighter. The asteroid is spherical, unlike the irregular shapes of smaller bodies with lower gravity. At its brightest it is still too dim to be seen with the naked eye.
On September 27, 2007, NASA launched the Dawn space probe to explore Ceres and Vesta. In 2015, Dawn became the first spacecraft to visit a dwarf planet, arriving at Ceres a few months before NASA's New Horizons spacecraft visited Pluto, another dwarf planet.
Ceres has an unusual crater Occator which contains bright salts.
Images[change | change source]
Related pages[change | change source]
References[change | change source]
- Ted Bowell, Bruce v (January 2, 2003). "Asteroid Observing Services". Lowell Observatory. Retrieved 2007-01-17.
- Yeomans, Donald K. (July 5, 2007). "1 Ceres". JPL Small-Body Database Browser. Retrieved 2007-07-05.—The listed values were rounded at the magnitude of uncertainty (1-sigma).
- "05. Dawn Explores Ceres Results from the Survey Orbit.pptx".
- Pitjeva, E.V. (2005). "High-Precision Ephemerides of Planets—EPM and Determination of Some Astronomical Constants" (PDF). Solar System Research 39 (3): 176. doi:10.1007/s11208-005-0033-2. http://iau-comm4.jpl.nasa.gov/EPM2004.pdf.
- D. T. Britt et al. Asteroid density, porosity, and structure, pp. 488 in Asteroids III, University of Arizona Press (2002).
- Thomas, P.C; Parker J.Wm.; McFadden, L.A.; et al. (2005). "Differentiation of the asteroid Ceres as revealed by its shape". Nature 437: 224-226. doi:10.1038/nature03938. http://adsabs.harvard.edu/abs/2005Natur.437..224T.
- Tedesco, E.F. (2004). "IRAS Minor Planet Survey. IRAS-A-FPA-3-RDR-IMPS-V6.0". NASA Planetary Data System. Retrieved 2007-03-15. Unknown parameter
- Neese, C. (2005). "Asteroid Taxonomy.EAR-A-5-DDR-TAXONOMY-V5.0". NASA Planetary Data System. Retrieved 2007-03-15. Unknown parameter
- Saint-Pé, O.; Combes, N.; Rigaut F. (1993). "Ceres surface properties by high-resolution imaging from Earth". Icarus 105: 271-281. doi:10.1006/icar.1993.1125. http://adsabs.harvard.edu/abs/1993Icar..105..271S.
- Piazzi, Giuseppe (1801). Risultati delle osservazioni della nuova Stella scoperta il dì 1 gennajo all'Osservatorio Reale di Palermo (in Italian). Palermo.
- Ceres at Solarviews.com
The Solar System
☾ = moon(s) ∅ = rings
|Mercury||Venus||Earth ☾||Mars ☾|
|Jupiter ☾ ∅||Saturn ☾ ∅||Uranus ☾ ∅||Neptune ☾ ∅|
|Dwarf planets||Ceres||Pluto ☾||Haumea ☾||Makemake|
|Groups and families: Vulcanoids · Near-Earth asteroids · Asteroid belt |
Jupiter Trojans · Centaurs · Neptune Trojans · Asteroid moons · Meteoroids · Pallas · Juno · Vesta · Hygiea · Interamnia · Europa
|See also the list of asteroids.|
|Kuiper belt – Plutinos: Orcus · Ixion – Cubewanos: Varuna · |
Quaoar · Huya
|Scattered disc: Sedna|
|Comets||Periodic comets and non-periodic comets |
Damocloids · Oort cloud
|See also the list of solar system objects|