Asteroid 809 Lundia (apparent magnitude 16.6) near a mag 15.6 star.
|Discovered by||Max Wolf|
|Discovery date||11 August 1915|
|MPC designation||(809) Lundia|
|1915 XP; 1936 VC|
|Epoch 31 July 2016 (JD 2457600.5)|
|Uncertainty parameter 0|
|Observation arc||100.48 yr (36700 d)|
|Aphelion||2.72316 AU (407.379 Gm)|
|Perihelion||1.84193 AU (275.549 Gm)|
|2.28254 AU (341.463 Gm)|
|3.45 yr (1259.6 d)|
Average orbital speed
|0° 17m 8.912s / day|
|Earth MOID||0.835871 AU (125.0445 Gm)|
|Jupiter MOID||2.69335 AU (402.919 Gm)|
|Jupiter Tisserand parameter||3.569|
|Dimensions||10.26 ± 0.07 km|
|Mass||(9.27 ± 3.09) × 1014 kg|
|1.64 ± 0.10 g/cm3|
Equatorial surface gravity
|0.001–0.003 m/s² (estimate)|
Equatorial escape velocity
|0.003–0.005 km/s (estimate)|
|15.4142 h (0.64226 d)|
max: 260-280 K
Lundia orbits within the Flora family. However, its V-type spectrum indicates that it is not genetically related to the Flora family, but rather is probably a fragment (two fragments, if its moon is included) ejected from the surface of 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 orbiting 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.
Lightcurve observations in 2005 revealed that Lundia is a binary system of two similarly sized objects orbiting their common centre of gravity. "Lundia" now refers to one of the objects, the other being provisionally designated S/2005 (809) 1. The similarity of size between the two components is suspected because during mutual occultations the brightness drops by a similar amount independently of which component is hidden. Due to the similar size of the primary and secondary the Minor Planet Center lists this as a binary companion.
Assuming an albedo similar to 4 Vesta (around 0.4) suggests that the components are about 7 km across. They orbit each other in a period of 15.4 hours, which roughly indicates that the separation between them is very close: to the order of 10–20 km if typical asteroid albedo and density values are assumed.
- "809 Lundia (1915 XP)". JPL Small-Body Database. NASA/Jet Propulsion Laboratory. Retrieved 4 May 2016.
- Carry, B. (December 2012), "Density of asteroids", Planetary and Space Science, 73, pp. 98–118, arXiv: , Bibcode:2012P&SS...73...98C, doi:10.1016/j.pss.2012.03.009. See Table 1.
- M. Florczak; D. Lazarro & R. Duffard (2002). "Discovering New V-Type Asteroids in the Vicinity of 4 Vesta". Icarus. 159: 178–182. Bibcode:2002Icar..159..178F. doi:10.1006/icar.2002.6913.
- V. Carruba, et al. (2005). "On the V-type asteroids outside the Vesta family". Astronomy & Astrophysics. 441 (2): 819–829. arXiv: . Bibcode:2005A&A...441..819C. doi:10.1051/0004-6361:20053355.
- Poznań observatory  (Lightcurve showing signature of the binary)
- "Satellites and Companions of Minor Planets". IAU / Central Bureau for Astronomical Telegrams. Archived from the original on 2011-01-21. Retrieved 2011-07-03.
- Electronic Telegram No. 239 announcing the binary system (2005 October 1)
- Discovery Circumstances: Numbered Minor Planets (1)-(5000) – Minor Planet Center
- (809) Lundia, datasheet, johnstonsarchive.net
- Asteroids with Satellites, Robert Johnston, johnstonsarchive.net
- Lightcurve showing signature of the binary
- 809 Lundia at the JPL Small-Body Database