194 Prokne
| Discovery | |
|---|---|
| Discovered by | C. H. F. Peters, 1879 |
| Discovery date | March 21, 1879 |
| Designations | |
| Main belt | |
| Orbital characteristics[1] | |
| Aphelion | 3.236 AU |
| Perihelion | 1.996 AU |
| 2.616 AU | |
| Eccentricity | 0.237 |
| 4.23 years | |
| Inclination | 18.50° |
| Physical characteristics | |
| Dimensions | 170.33±6.92 km[2] |
| Mass | (2.68±0.29)×1018 kg[2] |
Mean density | 1.03±0.16 g=cm3[2] |
| 15.679 h[3] | |
| Albedo | 0.053 |
Spectral type | C |
| 7.68 | |
|
| |
194 Prokne is a main-belt asteroid that was discovered by German-American astronomer C. H. F. Peters on March 21, 1879 in Clinton, New York, and named after Procne, the sister of Philomela in Greek mythology. Stellar occultations by Prokne have been observed twice, in 1984 from Italy and again in 1999 from Iowa (United States).
Observations from the W. M. Keck Observatory show the asteroid to be around 151 km across, with a size ratio of 1.13±0.06 between the major and minor axes. For comparison, observations by the IRAS observatory gave a diameter of 164 km.[4] The spectrum matches a classification of a C-type asteroid, indicating it has a primitive carbonaceous composition. Judging from radar data, the near surface solid density of the asteroid is 3.6+1.1
−0.9 g cm−3.[5]
Based upon a light curve that was generated from photometric observations of this asteroid at Pulkovo Observatory, it has a rotation period of 15.679±0.001 hours and varies in brightness by 0.16±0.02 in magnitude.[3]
References
- ↑ Yeomans, Donald K., "194 Prokne", JPL Small-Body Database Browser (NASA Jet Propulsion Laboratory), retrieved 2013-03-30.
- ↑ 2.0 2.1 2.2 Carry, B. (December 2012), "Density of asteroids", Planetary and Space Science 73: 98–118, arXiv:1203.4336, Bibcode:2012P&SS...73...98C, doi:10.1016/j.pss.2012.03.009. See Table 1.
- ↑ 3.0 3.1 Pilcher, Frederick (October 2011), "Rotation Period Determinations for 11 Parthenope, 38 Leda, 111 Ate 194 Prokne, 217 Eudora, and 224 Oceana", Bulletin of the Minor Planets Section of the Association of Lunar and Planetary Observers 38 (4): 183–185, Bibcode:2011MPBu...38..183P.
- ↑ Marchis, F. et al. (November 2006), "Shape, size and multiplicity of main-belt asteroids. I. Keck Adaptive Optics survey", Icarus 185 (1): 39–63, Bibcode:2006Icar..185...39M, doi:10.1016/j.icarus.2006.06.001, PMC 2600456, PMID 19081813.
- ↑ Magri, C. et al. (December 2001), "Radar constraints on asteroid regolith compositions using 433 Eros as ground truth", Meteoritics & Planetary Science 36 (12): 1697–1709, Bibcode:2001M&PS...36.1697M, doi:10.1111/j.1945-5100.2001.tb01857.x.
External links
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