847 Agnia
|
A three-dimensional model of 847 Agnia based on its light curve. | |
| Discovery | |
|---|---|
| Discovered by | G. N. Neujmin |
| Discovery site | Simeis |
| Discovery date | 2 September 1915 |
| Designations | |
| 1915 XX | |
| Orbital characteristics[1] | |
| Epoch 31 July 2016 (JD 2457600.5) | |
| Uncertainty parameter 0 | |
| Observation arc | 109.53 yr (40006 d) |
| Aphelion | 3.0472 AU (455.85 Gm) |
| Perihelion | 2.5158 AU (376.36 Gm) |
| 2.7815 AU (416.11 Gm) | |
| Eccentricity | 0.095516 |
| 4.64 yr (1694.4 d) | |
| 208.04° | |
| 0° 12m 44.892s / day | |
| Inclination | 2.4817° |
| 270.935° | |
| 130.341° | |
| Earth MOID | 1.52345 AU (227.905 Gm) |
| Jupiter MOID | 2.31009 AU (345.585 Gm) |
| Jupiter Tisserand parameter | 3.325 |
| Physical characteristics | |
Mean radius | 14.02±0.85 km |
| 14.827 h (0.6178 d) | |
| 0.1720±0.022 | |
| 10.29 | |
|
| |
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847 Agnia is a minor planet orbiting the Sun. It is approximately 28 kilometers in diameter.[2]
The spectrum of this object indicates that it is an S-type asteroid with both low and high calcium forms of pyroxene on the surface, along with less than 20% olivine. The high-calcium form of pyroxene forms 40% or more of the total pyroxene present, indicating a history of igneous rock deposits. This suggests that the asteroid underwent differentiation by melting, creating a surface of basalt rock.[3]
847 Agnia is the namesake of the Agnia family of asteroids that share similar orbital elements and physical properties. The members of this family, including 847 Agnia, most likely formed from the breakup of a basalt object, which in turn was spawned from a larger parent body that had previously undergone igneous differentiation. Other members of this family include 1020 Arcadia, 1228 Scabiosa, 2401 Aehlita, and 3395 Jitka[3]
Photometric observations of this asteroid collected during 2004–2005 show a rotation period of 14.827 ± 0.001 hours with a brightness variation of 0.45 ± 0.03 magnitude.[4]
References
- ↑ "847 Agnia (1915 XX)". JPL Small-Body Database. NASA/Jet Propulsion Laboratory. Retrieved 4 May 2016.
- ↑ IOTA/IOTA-ES occultation update for (847) Agnia
- 1 2 Sunshine, Jessica M.; et al. (August 2004), "High-calcium pyroxene as an indicator of igneous differentiation in asteroids and meteorites", Meteoritics & Planetary Science, 39 (8), pp. 1343–1357, Bibcode:2004M&PS...39.1343S, doi:10.1111/j.1945-5100.2004.tb00950.x.
- ↑ Pray, Donald P. (September 2005), "Lightcurve analysis of asteroids 106, 752, 847, 1057, 1630, 1670, 1927 1936, 2426, 2612, 2647, 4087, 5635, 5692, and 6235", The Minor Planet Bulletin, 32 (3): 48–51, Bibcode:2005MPBu...32...48P.
