1527 Malmquista
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Lightcurve-based 3D-model of Malmquista
|
|
| Discovery | |
|---|---|
| Discovered by | Y. Väisälä |
| Discovery site | Turku Obs. |
| Discovery date | 18 October 1939 |
| Designations | |
| MPC designation | (1527) Malmquista |
|
Named after
|
Gunnar Malmquist (astronomer) |
| 1939 UG · 1929 TG 1932 OB · 1972 TK A909 TC |
|
| main-belt · Flora | |
| Orbital characteristics | |
| Epoch 16 February 2017 (JD 2457800.5) | |
| Uncertainty parameter 0 | |
| Observation arc | 87.47 yr (31,948 days) |
| Aphelion | 2.6695 AU |
| Perihelion | 1.7843 AU |
| 2.2269 AU | |
| Eccentricity | 0.1987 |
| 3.32 yr (1,214 days) | |
| 144.63° | |
| 0° 17m 47.76s / day | |
| Inclination | 5.1939° |
| 16.133° | |
| 304.52° | |
| Physical characteristics | |
| Dimensions |
9.55±0.49 km 10.040±0.134 km 10.338±0.071 km 10.80 km (calculated) |
|
14.044±0.0244 h 14.0591 h 14.077±0.004 h |
|
|
0.2202±0.0169 0.24 (assumed) 0.307±0.037 |
|
| S | |
| 12.0 · 12.2 · 12.481±0.002 (S) | |
1527 Malmquista, provisional designation 1939 UG, is a stony Florian asteroid from the inner regions of the asteroid belt, approximately 10 kilometers in diameter.
It was discovered on 18 October 1939, by Finnish astronomer Yrjö Väisälä at Turku Observatory in Southwest Finland. It was named for the Swedish astronomer Gunnar Malmquist.
Malmquista is a member of the Flora family, one of the largest families of stony asteroids in the main belt. It orbits the Sun in the inner main-belt at a distance of 1.8–2.7 AU once every 3 years and 4 months (1,214 days). Its orbit has an eccentricity of 0.20 and an inclination of 5° with respect to the ecliptic. In 1909, it was first observed at Heidelberg Observatory as A909 TC. The body's observation arc begins at Lowell Observatory in 1929, when it was identified as 1929 TG, 10 years prior to its official discovery observation at Turku.
In September 2002, a first rotational lightcurve of Malmquista was obtained from photometric observations by Stephen Brincat at Flarestar Observatory on the island of Malta. Lightcurve analysis gave a well-defined rotation period of 14.077 hours with a brightness variation of 0.60 magnitude (U=3). In September 2012, observations at the Palomar Transient Factory, California, gave a period of 14.044 hours and an amplitude of 0.42 magnitude (U=2).
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