6489 Golevka
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|
| Discovery | |
|---|---|
| Discovered by | Eleanor F. Helin |
| Discovery date | May 10, 1991 |
| Designations | |
| 1991 JX | |
| Alinda, Apollo, PHA,[1] Mars-crosser |
|
| Orbital characteristics | |
| Epoch 2001-Sep-14 (JD 2452166.5) | |
| Aphelion | 4.022147 AU (601.7 Gm) |
| Perihelion | 0.994779 AU (147.6 Gm) |
| 2.508463 AU (373.9 Gm) |
|
| Eccentricity | 0.603431 |
| 3.97 a (1451.142 d) | |
|
Average orbital speed
|
16.980 km/s |
| 200.782705° | |
| Inclination | 2.279886° |
| 211.760841° | |
| 65.734166° | |
| Physical characteristics | |
| Dimensions | 0.53 km[1] |
| Mass | 2.10 × 1011 kg |
|
Mean density
|
2.7+0.4 −0.6 g/cm³ |
| 0.0002 m/s² | |
| 0.0003 km/s | |
| 6.026 hr[1] | |
| Albedo | 0.151[1] |
| Temperature | ~176 K |
|
Spectral type
|
Q |
| 19.2[1] | |
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6489 Golevka is an Apollo, Mars-crosser, and Alinda asteroid discovered in 1991 by Eleanor F. Helin.
Its name has a complicated origin. In 1995, Golevka was studied simultaneously by three radar observatories across the world: Goldstone in California, Yevpatoria RT-70 radio telescope in Ukraine (Yevpatoria is sometimes romanized as Evpatoria) and Kashima in Japan. 'Golevka' comes from the first few letters of each observatory's name; it was proposed by the discoverer following a suggestion by Alexander L. Zaitsev.
Golevka is a small object, measuring 0.6 × 1.4 km. The radar observations revealed that it has a very strange, angular shape that looks different depending on the direction. In 2003 the Yarkovsky effect was first observed at work by high-precision radar observations of Golevka.[2] Between 1991 and 2003, the small force of the Yarkovsky Effect caused a shift of 15 kilometers (9.4 miles) from what would be expected based on only gravitational interactions.[2] This helped evaluate the asteroid's bulk density (2.7 ± 0.5 g/cm³) and mass (2.10×1011 kg).
Golevka approaches Earth to 0.05 AU (7,500,000 km; 4,600,000 mi) in 2046, 0.10 AU in 2069, and 0.11 AU in 2092.[3] On the other hand, Golevka's collision probability with any planet is negligible for at least the next nine centuries.[4] Its orbit is strikingly similar to that of 4179 Toutatis in eccentricity, semi-major axis, and inclination. However, Toutatis is better known due to a close approach to Earth in 2004.
References
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