3850 Peltier
| Discovery | |
|---|---|
| Discovered by | E. Bowell |
| Discovery site | Anderson Mesa Stn. |
| Discovery date | 7 October 1986 |
| Designations | |
| MPC designation | 3850 Peltier |
|
Named after
|
Leslie Peltier (astronomer) |
|
1986 TK2 · 1949 PC 1969 OC1 · 1979 OX13 1982 OW |
|
| main-belt · Flora | |
| Orbital characteristics | |
| Epoch 16 February 2017 (JD 2457800.5) | |
| Uncertainty parameter 0 | |
| Observation arc | 47.25 yr (17,259 days) |
| Aphelion | 2.5969 AU |
| Perihelion | 1.8721 AU |
| 2.2345 AU | |
| Eccentricity | 0.1622 |
| 3.34 yr (1,220 days) | |
| 67.773° | |
| 0° 17m 42.36s / day | |
| Inclination | 5.2684° |
| 124.13° | |
| 207.35° | |
| Physical characteristics | |
| Dimensions | 4.00 km (calculated) |
|
2.4287±0.0002 h 2.4289±0.0001 h |
|
| 0.4 (assumed) | |
| SMASS = V · V | |
| 13.6 · 13.62±0.37 | |
3850 Peltier, provisional designation 1986 TK2, is a Florian asteroid and suspected interloper from the inner regions of the asteroid belt, approximately 4 kilometers in diameter. It was discovered on 7 October 1986, by American astronomer Edward Bowell at Lowell's Anderson Mesa Station, near Flagstaff, Arizona. It is named for astronomer Leslie Peltier.
In the SMASS taxonomy, Peltier is a V-type asteroid but possesses the orbital characteristics of a member of the Flora family, which is one of the largest groups of stony S-type asteroids in the main-belt. It is therefore thought to be an unrelated interloper that does not origin from the Flora family's parent body. Peltier orbits the Sun at a distance of 1.9–2.6 AU once every 3 years and 4 months (1,220 days). Its orbit has an eccentricity of 0.16 and an inclination of 5° with respect to the ecliptic. In 1949, it was first identified as 1949 PC at Johannesburg. The body's observation arc begins at Crimea-Nauchnij in 1979, when it was identified as 1979 OX13, 10 years prior to its official discovery observation at Anderson Mesa.
A rotational light-curve of Peltier was obtained by Czech astronomer Petr Pravec at Ondřejov Observatory in October 2006. Lightcurve analysis gave a rotation period of 2.4287 hours with a brightness variation of 0.09 magnitude (U=2). In December 2013, photometric observations by Australian amateur astronomer Julian Oey gave a concurring period of 2.4289 hours and an amplitude of 0.10 magnitude (U=3).
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