_Eger.png) Shape model ofEger from itslightcurve | |
| Discovery | |
|---|---|
| Discovered by | M. Lovas |
| Discovery site | Piszkéstető |
| Discovery date | 20 January 1982 |
| Designations | |
| (3103) Eger | |
Named after | Eger |
| 1982 BB | |
| 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) | |
| 208.62° | |
| 0° 35m 31.92s / day | |
| Inclination | 20.931° |
| 129.792° | |
| 254.007° | |
| Earth MOID | 0.0778981 AU (11.65339 Gm) |
| Proper orbital elements[1][2] | |
Propereccentricity | 0.325 |
Properinclination | 22.364° |
Propermean motion | 99.460 deg / yr |
Properorbital period | 3.61955yr (1322.039d) |
| Physical characteristics | |
| 1.5 km[1] | |
| 5.710156±0.000007 h[3] | |
| 0.64[1] | |
| E | |
| 15.38[1] | |
3103 Eger is anApollo andMars-crosser asteroid that was discovered in 1982, byMiklós Lovas. It was named after the city ofEger,Hungary. It has analbedo of 0.64,[1] making it a highly reflective asteroid.
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It has made and will continue to make many close approaches to Earth. Its closest approach occurred on 6 August 1996, when the asteroid passed 0.11509 AU (17.217 Gm) from Earth.[1] The observedYORP value is(1.4±0.6)×10−8 rad d−2.[3]
3103 Eger is the only asteroid besides4 Vesta identified as the parent body for specific meteorites. 4 Vesta is the parent body forHowardite,Eucrite, andDiogenite meteorites, while 3103 Eger is the parent body forAubrite meteorites. In this characteristic 3103 Eger is related spectroscopically to the434 Hungaria type asteroids, which are a Hirayama-family of orbital types, andE-type asteroids which form a spectroscopical type.
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