809 Lundia
Encyclopedia : 8 : 80 : 809 : 809 Lundia
| Orbital elements | |
|---|---|
| Eccentricity (orbit)>e | |
| Inclination>i | ° |
| Perihelion>q |
|
| Argument of perihelion>ω | ° |
| Semi-major axis>a | AU |
| Longitude of the ascending node>ω | ° |
| Aphelion>Q |
|
| Mean anomaly>M | ° |
| Orbital period>P | years |
| Mean motion>n | °/day |
| Time of perihelion passage>TP | |
809 Lundia is a small, binary, V-type asteroid orbiting within the Flora family in the Main Belt.
The V-type spectrum indicates that it is not genetically related to the Flora family, but rather is probably a fragment (actually two fragments) ejected off the surface of nearby 4 Vesta by a large impact in the past. Its orbit lies too far from Vesta for it to actually be a member of the Vesta family It is not clear how it arrived at an orbit so far from Vesta, but other examples of V-type asteroids fairly far from their parent body are known. A mechanism of interplay between the Yarkovsky effect and nonlinear secular resonances (primarily involving Jupiter and Saturn) has been proposed
Binary
A satellite, designated S/2005 (809) 1, was identified based on lightcurve observations in 2005. In fact, the size of the two components appear to be similar, because during mutual occultations the brightness drops by a similar amount independently of which component is hidden Poznań observatory [link] (Lightcurve showing signature of the binary). Assuming an albedo similar to 4 Vesta (around 0.4), suggests that the components are about 7 km across. They orbit each other with a period of 15.4 hours, which roughly indicates that the binary is very close — the separation being of the order of 10-20 km, if typical asteroid albedo and density values are assumed.References
External links
- [Discovery Circumstances: Numbered Minor Planets]
- [Johnston Archive entry for 809 Lundia]
- [Lightcurve showing signature of the binary]
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