1575 Winifred
| Discovery | |
|---|---|
| Discovered by |
Indiana University (Indiana Asteroid Program) |
| Discovery site | Goethe Link Obs. |
| Discovery date | 20 April 1950 |
| Designations | |
| MPC designation | 1575 Winifred |
|
Named after
|
Winifred Sawtelle (staff member at USNO) |
| 1950 HH · 1928 HG 1939 GK · 1950 HD1 1977 UH1 |
|
| main-belt · Phocaea | |
| Orbital characteristics | |
| Epoch 16 February 2017 (JD 2457800.5) | |
| Uncertainty parameter 0 | |
| Observation arc | 88.33 yr (32,261 days) |
| Aphelion | 2.7988 AU |
| Perihelion | 1.9491 AU |
| 2.3739 AU | |
| Eccentricity | 0.1790 |
| 3.66 yr (1,336 days) | |
| 104.71° | |
| 0° 16m 10.2s / day | |
| Inclination | 24.827° |
| 206.84° | |
| 348.35° | |
| Physical characteristics | |
| Dimensions |
9.31±1.0 km (IRAS) 9.441±0.131 km 9.45 km (derived) 9.488±0.254 10.66±0.43 km |
|
125±2 h 129 h |
|
|
0.236±0.033 0.2388±0.0311 0.2452±0.064 0.247±0.034 0.3134 (derived) |
|
| S | |
| 11.36±1.19 · 12.0 · 12.3 | |
1575 Winifred, provisional designation 1950 HH, is a stony Phocaea asteroid and slow rotator from the inner regions of the asteroid belt, approximately 9.5 kilometers in diameter. It was discovered on 20 April 1950, by astronomer R. C. Cameron of Indiana University during the Indiana Asteroid Program at Goethe Link Observatory in Indiana, United States.
The stony S-type asteroid is a member of the Phocaea family, a group of asteroids with similar orbital characteristics, named after the family's namesake 25 Phocaea. It orbits the Sun at a distance of 1.9–2.8 AU once every 3 years and 8 months (1,336 days). Its orbit has an eccentricity of 0.18 and an inclination of 25° with respect to the ecliptic.Winifred was first identified as 1928 HG at Johannesburg Observatory in 1928, extending the body's observation arc by 22 years prior to its official discovery observation.
In July 2009, a rotational light-curve was obtained for this asteroid from photometric observations taken by American astronomer Brian D. Warner at his Palmer Divide Observatory in Colorado. It gave a well-defined rotation period of 125±2 hours with an exceptionally high brightness amplitude of 1.20 in magnitude (U=3), and no sign of a non-principal axis rotation (NPAR). The result supersedes a previous observation by French astronomer Laurent Bernasconi from May 2005, that gave a similar, yet less accurate period of 129 hours, and with a smaller amplitude of 0.51 in magnitude (U=1).
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