809 Lundia

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809 Lundia
809Lun-LB1-mag17.jpg
Asteroid 809 Lundia (apparent magnitude 16.6) near a mag 15.6 star
Discovery
Discovered by Max Wolf
Discovery date11 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
Dimensions10.26 ± 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.

    Contents

    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.

    Related Research Articles

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    <span class="mw-page-title-main">1338 Duponta</span>

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    2478 Tokai, provisionally designated 1981 JC, is a stony Florian asteroid and binary system from the inner regions of the asteroid belt, approximately 10 kilometers in diameter. It was discovered on 4 May 1981, by Japanese astronomer Toshimasa Furuta at Tōkai Observatory, Japan. The asteroid was named after the city of Tōkai.

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    3982 Kastelʹ, provisional designation 1984 JP1, is a Florian asteroid and a suspected binary system from the inner regions of the asteroid belt, approximately 6.9 kilometers in diameter.

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    10208 Germanicus, provisional designation 1997 QN1, is a stony Florian asteroid and binary system from the inner regions of the asteroid belt, approximately 3.5 kilometers in diameter.

    20325 Julianoey, provisional designation 1998 HO27, is a Vestian asteroid and a synchronous binary system from the inner regions of the asteroid belt, approximately 5 kilometers (3 miles) in diameter. It was discovered on 21 April 1998, by astronomers of the Spacewatch survey at Kitt Peak National Observatory near Tucson, Arizona. The asteroid was named after Australian photometrist Julian Oey. The discovery of its minor-planet moon was announced in December 2014.

    32008 Adriángalád, provisional designation: 2000 HM53, is a background asteroid and synchronous binary system from the inner regions of the asteroid belt, approximately 4 kilometers (2.5 miles) in diameter. It was discovered on 29 April 2000, by astronomers with the LINEAR program at Lincoln Laboratory's Experimental Test Site near Socorro, New Mexico, in the United States. The V-type asteroid has a rotation period of 3.0 hours. It was named for Slovak astronomer Adrián Galád. Its 1.6-kilometer sized minor-planet moon was discovered in August 2007.

    References

    1. ↑ "809 Lundia (1915 XP)". JPL Small-Body Database . NASA/Jet Propulsion Laboratory . Retrieved 4 May 2016.
    2. 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.
    3. ↑ 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.
    4. ↑ 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.
    5. 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)
    6. ↑ "Satellites and Companions of Minor Planets". IAU / Central Bureau for Astronomical Telegrams. Archived from the original on 21 January 2011. Retrieved 3 July 2011.
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