Discovery | |
---|---|
Discovered by | Max Wolf |
Discovery date | 11 August 1915 |
Designations | |
(809) Lundia | |
Pronunciation | /ˈlʌndiə/ |
Named after | Lund Observatory |
1915 XP; 1936 VC | |
Main belt | |
Orbital characteristics[1] | |
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) | |
Eccentricity | 0.19304 |
3.45 yr (1259.6 d) | |
76.7867° | |
0° 17m 8.912s / day | |
Inclination | 7.14911° |
154.580° | |
196.162° | |
Physical characteristics | |
Dimensions | 10.26 ± 0.07 km[2] |
Mass | (9.27 ± 3.09) × 1014 kg[2] |
Mean density | 1.64 ± 0.10 g/cm3[2] |
15.4142 h (0.64226 d) | |
V | |
12.2 | |
809 Lundia is a small, binary, V-type asteroid[3] orbiting within the Flora family in the main belt. It is named after Lund Observatory, Sweden.
Characteristics
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.[4]
Binary system
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.[5] Due to the similar size of the primary and secondary the Minor Planet Center lists this as a binary companion.[6]
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,[5] 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.
References
- ↑ "809 Lundia (1915 XP)". JPL Small-Body Database. NASA/Jet Propulsion Laboratory. Retrieved 4 May 2016.
- 1 2 3 Carry, B. (December 2012), "Density of asteroids", Planetary and Space Science, vol. 73, pp. 98–118, arXiv:1203.4336, 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:astro-ph/0506656. Bibcode:2005A&A...441..819C. doi:10.1051/0004-6361:20053355.
- 1 2 Poznań observatory "Physical studies of asteroids at Poznan Observatory". Archived from the original on 2 July 2001. Retrieved 2 July 2001. (Lightcurve showing signature of the binary)
- ↑ "Satellites and Companions of Minor Planets". IAU / Central Bureau for Astronomical Telegrams. Archived from the original on 21 January 2011. Retrieved 3 July 2011.
External links
- 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 AstDyS-2, Asteroids—Dynamic Site
- 809 Lundia at the JPL Small-Body Database