2296 Kugultinov
| Discovery | |
|---|---|
| Discovered by | L. Chernykh |
| Discovery site | Crimea–Nauchnij |
| Discovery date | 18 January 1975 |
| Designations | |
| MPC designation | 2296 Kugultinov |
|
Named after
|
David Kugultinov (Soviet poet) |
|
1975 BA1 · 1941 FM 1958 DF · 1975 CE 1978 RM1 |
|
| main-belt · Themis | |
| Orbital characteristics | |
| Epoch 16 February 2017 (JD 2457800.5) | |
| Uncertainty parameter 0 | |
| Observation arc | 75.24 yr (27,482 days) |
| Aphelion | 3.7113 AU |
| Perihelion | 2.6500 AU |
| 3.1806 AU | |
| Eccentricity | 0.1668 |
| 5.67 yr (2,072 days) | |
| 145.79° | |
| 0° 10m 25.68s / day | |
| Inclination | 1.2545° |
| 42.234° | |
| 100.13° | |
| Physical characteristics | |
| Dimensions | 21.48 km (calculated) 21.566±0.067 km |
|
8.43±0.02 h 10 h 16.850±0.004 h |
|
| 0.08 (assumed) 0.083±0.004 |
|
| C | |
| 11.6 · 11.7 · 11.77±0.23 | |
2296 Kugultinov, provisional designation 1975 BA1, is a carbonaceous Themistian asteroid from the outer region of the asteroid belt, approximately 22 kilometers in diameter. It was discovered on 18 January 1975, by Russian astronomer Lyudmila Chernykh at the Crimean Astrophysical Observatory on the Crimean peninsula in Nauchnyj.
The C-type asteroid is a member of the Themis family, a dynamical family of outer-belt asteroids with nearly coplanar ecliptical orbits. It orbits the Sun at a distance of 2.7–3.7 AU once every 5 years and 8 months (2,072 days). Its orbit has an eccentricity of 0.17 and an inclination of 1° with respect to the ecliptic.
According to the space-based survey carried out by the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer, the asteroid measures 21.6 kilometers in diameter and its surface has an albedo of 0.083, while the Collaborative Asteroid Lightcurve Link (CALL) assumes an albedo of 0.08 and calculates a diameter of 21.5 kilometers, based on an absolute magnitude of 11.7.
Three different rotational light-curves for this asteroid were obtain from photometric observations. The first, fragmentary light-curve by Roberto Crippa and Federico Manzini in December 2013, gave a rotation period of 10 hours with a brightness variation of 0.03 in magnitude (U=1). In April 2015, the result was superseded by observations made by Kim Lang at the Klokkerholm Observatory in Denmark, and by a team at the U.S. University of Maryland using the iTelescope network, obtaining a period of 16.850±0.004 (U=2) and 8.4332±0.0224 hours (U=2+) with an amplitude of 0.23 and 0.19, respectively. CALL considers the shorter period solution the better result.
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