3103 Eger
.png) A three-dimensional model of 3103 Eger based on its light curve | |||||||||
| Discovery | |||||||||
|---|---|---|---|---|---|---|---|---|---|
| Discovered by | Miklós Lovas | ||||||||
| Discovery site | Piszkesteto | ||||||||
| Discovery date | 20 January 1982 | ||||||||
| Designations | |||||||||
Named after | Eger | ||||||||
| 1982 BB | |||||||||
| Apollo, Mars crosser | |||||||||
| Orbital characteristics[1] | |||||||||
| Epoch 13 January 2016 (JD 2457400.5) | |||||||||
| Uncertainty parameter 0 | |||||||||
| Observation arc | 12495 days (34.21 yr) | ||||||||
| Aphelion | 1.9021 AU (284.55 Gm) | ||||||||
| Perihelion | 0.90673 AU (135.645 Gm) | ||||||||
| 1.4044 AU (210.10 Gm) | |||||||||
| Eccentricity | 0.35437 | ||||||||
| 1.66 yr (607.90 d) | |||||||||
Average orbital speed | 40.496 km/s | ||||||||
| 208.62° | |||||||||
| 0° 35m 31.92s / day | |||||||||
| Inclination | 20.931° | ||||||||
| 129.792° | |||||||||
| 254.007° | |||||||||
| Earth MOID | 0.0778981 AU (11.65339 Gm) | ||||||||
| Jupiter MOID | 3.70058 AU (553.599 Gm) | ||||||||
| TJupiter | 4.613 | ||||||||
| Proper orbital elements | |||||||||
Proper eccentricity | 0.325 | ||||||||
Proper inclination | 22.364° | ||||||||
Proper mean motion | 99.460 deg / yr | ||||||||
Proper orbital period | 3.61955 yr (1322.039 d) | ||||||||
| Physical characteristics | |||||||||
| Dimensions | 1.5 km[1] | ||||||||
| 0.75 km | |||||||||
| 5.7059 h (0.23775 d)[1] | |||||||||
| 0.64[1] | |||||||||
| |||||||||
| E | |||||||||
| 15.38[1] | |||||||||
3103 Eger is an Apollo and Mars-crosser asteroid that was discovered in 1982, by Miklós Lovas. It was named after the city of Eger, Hungary. It has an albedo of 0.64,[1] making it a highly reflective asteroid.
It has made and will continue to make many close approaches to Earth. Its closest so far occurred in August 6, 1996, when the asteroid passed 0.11509 AU (17.217 Gm) from Earth.[1]
3103 Eger is the only asteroid besides 4 Vesta identified as the parent body for specific meteorites. 4 Vesta is the parent body for Howardite, Eucrite, and Diogenite meteorites, while 3103 Eger is the parent body for Aubrite meteorites. In this characteristic 3103 Eger is related spectroscopically to the 434 Hungaria type asteroids, which are a Hirayama-family of orbital types, and E-type asteroids which form a spectroscopical type.
See also
References
- ^ a b c d e f g h "3103 Eger". JPL Small-Body Database. Jet Propulsion Laboratory. SPK-ID: 3103. Retrieved 14 April 2016.
- ^ "Planetary Habitability Calculators". Planetary Habitability Laboratory. University of Puerto Rico at Arecibo. Retrieved 27 November 2015.
- ^ "(162058) 1997AE12". NEODyS. University of Pisa. Retrieved 25 November 2015.
External links
- Mineralogy of Asteroids
- Relation between E-asteroids, 3103 Eger and 434 Hungaria
- Relations between E-type asteroids 2867 Šteins, a target of the Rosetta mission, and 3103 Eger
- 3103 Eger in the Ondrejov NEO program
- Benner, et al. - Radar Detection of Near-Earth Asteroids 2062 Aten, 2101 Adonis, 3103 Eger, 4544 Xanthus, and 1992 QN (1997)
- 3103 Eger at the JPL Small-Body Database
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