21 Lutetia: Difference between revisions
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* [http://www.rni.helsinki.fi/~mjk/thirty.pdf Shape model deduced from lightcurve] |
* [http://www.rni.helsinki.fi/~mjk/thirty.pdf Shape model deduced from lightcurve] |
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* [http://ssd.jpl.nasa.gov/horizons.cgi?find_body=1&body_group=sb&sstr=21 JPL Ephemeris] |
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* [http://www.spaceflightnow.com/news/n1007/10lutetia/ Rosetta snaps views of asteroid Lutetia] |
* [http://www.spaceflightnow.com/news/n1007/10lutetia/ Rosetta snaps views of asteroid Lutetia] |
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* [http://www.nasa.gov/topics/solarsystem/features/rosetta_images20100710.html Rosetta's full resolution images of Lutetia] |
* [http://www.nasa.gov/topics/solarsystem/features/rosetta_images20100710.html Rosetta's full resolution images of Lutetia] |
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Revision as of 02:53, 22 December 2013
| File:Lutetia closest approach (Rosetta).jpg Rosetta image of 21 Lutetia at closest approach | |
| Discovery | |
|---|---|
| Discovered by | Hermann M. S. Goldschmidt |
| Discovery date | November 15, 1852 |
| Designations | |
| Pronunciation | /ljuːˈtiːʃə/ lew-TEE-shə |
Named after | Paris (Latin: Lutētia) |
| Main belt | |
| Orbital characteristics[1] | |
| Epoch January 30, 2005 (JD 2453400.5) | |
| Aphelion | 2.834 AU (423.955 Gm) |
| Perihelion | 2.036 AU (304.600 Gm) |
| 2.435 AU (364.277 Gm) | |
| Eccentricity | 0.164 |
| 3.80 a (1387.902 d) | |
Average orbital speed | 18.96 km/s |
| 75.393° | |
| Inclination | 3.064° |
| 80.917° | |
| 250.227° | |
| Physical characteristics | |
| Dimensions | (121± 1) × (101 ± 1) × (75 ± 13) km[2] |
| Volume | 5.0 ± 0.4×1014 m³[3] |
| Mass | 1.700 ± 0.017×1018 kg[3] |
Mean density | 3.4 ± 0.3 g/cm³[3] |
| ~0.049 m/s² | |
| ~0.069 km/s | |
| 0.3402 d (8.1655 h)[1] | |
| 96°[2] | |
North pole right ascension | 51.8 ± 0.4°[2] |
North pole declination | +10.8 ± 0.4°[2] |
| Albedo | 0.19 ± 0.01 (geometrical)[2] 0.073 ± 0.002 (bond)[2] |
| Temperature | 170–245 K[4] |
Spectral type | M[1] |
| 9.25[5] to 13.17 | |
| 7.29[6] | |
.jpg){kind=link}
21 Lutetia is a large main-belt asteroid of an unusual spectral type. It measures about 100 kilometers in diameter (120 km along its major axis). It was discovered in 1852 by Hermann Goldschmidt, and is named after Lutetia, the Latin name of the city that stood where Paris was later built.
Lutetia has an irregular shape and is heavily cratered, with the largest impact crater reaching 45 km in diameter. The surface is geologically heterogeneous and is intersected by a system of grooves and scarps, which are thought to be fractures. It has a high average density, meaning that it is made of metal-rich rock.
The Rosetta probe passed within 3,162 km (1,965 mi) of Lutetia in July 2010.[7] It was the largest asteroid visited by a spacecraft until the Dawn mission arrived at 4 Vesta in July 2011.
Discovery and exploration
Lutetia was discovered on November 15, 1852, by Hermann Goldschmidt from the balcony of his apartment in Paris.[8][9] A preliminary orbit for the asteroid was computed in November–December 1852 by German astronomer Georg Rümker and others.[10] In 1903, it was photographed at opposition by Edward Pickering at Harvard College Observatory. He computed an opposition magnitude of 10.8.[11]
There have been two reported stellar occultations by Lutetia, observed from Malta in 1997 and Australia in 2003, with only one chord each, roughly agreeing with IRAS measurements.[citation needed]
On July 10, 2010, the European Rosetta space probe flew by Lutetia at a minimum distance of 3168 ± 7.5 and a velocity of 15 kilometres per second on its way to the comet 67P/Churyumov-Gerasimenko.[3] The flyby provided images of up to 60 meters per pixel resolution and covered about 50% of the surface, mostly in the northern hemisphere.[2][7] The 462 images were obtained in 21 narrow and broad band filters extending from 0.24 to 1 μm.[7] Lutetia was also observed by the visible–near-infrared imaging spectrometer VIRTIS, and measurements of the magnetic field and plasma environment were taken as well.[2][7]
Characteristics
Orbit
Lutetia orbits the Sun at the distance of approximately 2.4 AU in the inner asteroid belt. Its orbit lies almost in the plane of ecliptic and is moderately eccentric. The orbital period of Lutetia is 3.8 years.[12]
Mass and density
The Rosetta flyby demonstrated that the mass of Lutetia is (1.700 ± 0.017)×1018 kg,[3] smaller than the pre-flyby estimate of 2.57×1018 kg.[13] It has one of the highest densities seen before in asteroids at 3.4 ± 0.3 g/cm3.[2] Taking into account possible porosity of 10–15%, the bulk density of Lutetia exceeds that of a typical stony meteorite.[3]
Composition
The composition of Lutetia has puzzled astronomers for some time. While classified among the M-type asteroids,[1] most of which are metallic, Lutetia is one of the anomalous members that do not display much evidence of metal on their surface. Indeed, there were various indications of a non-metallic surface: a flat, low frequency spectrum similar to that of carbonaceous chondrites and C-type asteroids and not at all like that of metallic meteorites,[14] a low radar albedo unlike the high albedos of strongly metallic asteroids like 16 Psyche,[6] evidence of hydrated materials on its surface,[15] abundant silicates,[16] and a thicker regolith than most asteroids.[17]
The Rosetta probe actually found that the asteroid has a moderately red spectrum in the visible light and essentially flat spectrum in the near infrared. No absorption features were detected in the whole wavelength range covered by observations—0.4–3.5 μm. Thus previous reports of hydrated minerals and organic compounds on the surface of Lutetia have been disproven. The surface also does not contain any olivine. Together with the high density of Lutetia these results indicate that it is either made of the enstatite chondrite material or may be related to metal-rich and water-poor carbonaceous chondrite of classes like CB, CH, or CR.[4][18]
Rosetta observations revealed that the surface of Lutetia is covered with a regolith made of loosely aggregated dust particles 50–100 μm in size. It is estimated to be 3 km thick and may be responsible for the softened outlines of many of the larger craters.[2][7]
Shape and axial tilt
The Rosetta probe's photographs confirmed the results of a 2003 lightcurve analysis that described Lutetia as a rough sphere with "sharp and irregular shape features".[19] A study carried out by I.N. Belskaya et al. in 2004–2009 had proposed that "Lutetia has a non-convex shape, probably due to a large crater";[20] it is not yet clear whether Rosetta's findings support this claim.
The analysis of Rosetta images in combination with photometric light curves yielded the position of the north rotational pole of Lutetia: RA= – 51.8 ± 0.4; Dec= – +10.8 ± 0.4°. This gives an axial tilt of 96° (retrograde rotator), meaning that the axis of rotation is approximately parallel to the ecliptic, similar to the planet Uranus.[2]
Surface features and nomenclature
Surface features
The surface of Lutetia is covered by numerous impact craters and intersected by fractures, scarps and grooves thought to be surface manifestations of internal fractures. On the imaged hemisphere of the asteroid there are a total of 350 craters with diameters ranging from 600 m to 55 km. The most heavily cratered surfaces (in Achaia region) have a crater retention age of about 3.6 ± 0.1 billion years.[2]
The surface of Lutetia has been divided into seven regions based on their geology. They are Baetica (Bt), Achaia (Ac), Etruria (Et), Narbonensis (Nb), Noricum (Nr), Pannonia (Pa), and Raetia (Ra). The Baetica region is situated around the north pole (in the center of the image) and includes a cluster of impact craters 21 km in diameter as well as their impact deposits. It is the youngest surface unit on Lutetia. Baetica is covered by a smooth ejecta blanket approximately 600 m thick that has partially buried older craters. Other surface features include landslides, gravitational taluses and ejecta blocks up to 300 m in size. The landslides and corresponding rock outcrops are correlated with variations of albedo, being generally brighter.[2]
The two oldest regions are Achaia and Noricum. The former is a remarkably flat area with a lot of impact craters. The Narbonensis region coincides with the largest impact crater on Lutetia—Massilia. It includes a number of smaller units and is modified by pit chains and grooves formed at a later epoch. Other two regions—Pannonia and Raetia are also likely to be large impact craters. The last Noricum region is intersected by a prominent groove 10 km in length and about 100 m deep.[2]
The numerical simulations showed that even the impact that produced the largest crater on Lutetia, which is 45 km in diameter, seriously fractured but did not shatter the asteroid. So, Lutetia has likely survived intact from the beginning of the Solar System. The existence of linear fractures and the impact crater morphology also indicate that the interior of this asteroid has a considerable strength and is not a rubble pile like many smaller asteroids. Taken together, these facts suggest that Lutetia should be classified as a primordial planetesimal.[2]
Nomenclature
In March, 2011, the Working Group for Planetary Nomenclature at the International Astronomical Union agreed on a naming scheme for geographical features on Lutetia. Since Lutetia was a Roman city, the asteroid's craters are named after cities of the Roman Empire and the adjacent parts of Europe during the time of Lutetia's existence. Its regions are named after the discoverer of Lutetia (Goldschmidt) and after provinces of the Roman Empire at the time of Lutetia. Other features are named after rivers of the Roman Empire and the adjacent parts of Europe at the time of Lutetia.[21]
References
- ^ a b c d "JPL Small-Body Database Browser: 21 Lutetia". 2010-06-13 last obs. Retrieved 2008-12-07.
{{cite web}}: Check date values in:|date=(help) - ^ a b c d e f g h i j k l m n o p Attention: This template ({{cite doi}}) is deprecated. To cite the publication identified by doi:10.1126/science.1207325, please use {{cite journal}} (if it was published in a bona fide academic journal, otherwise {{cite report}} with
|doi=10.1126/science.1207325instead. - ^ a b c d e f M. Pätzold, T. P. Andert, S. W. Asmar, J. D. Anderson, J.-P. Barriot, M. K. Bird1, B. Häusler, M. Hahn, S. Tellmann, H. Sierks, P. Lamy, B. P. Weiss (October 28, 2011). "Asteroid 21 Lutetia: Low Mass, High Density". 334 (6055). Science Magazine: 491–2. Bibcode:2011Sci...334..491P. doi:10.1126/science.1209389. Retrieved 2011-10-28.
{{cite journal}}: Cite journal requires|journal=(help)CS1 maint: multiple names: authors list (link) CS1 maint: numeric names: authors list (link) - ^ a b Attention: This template ({{cite doi}}) is deprecated. To cite the publication identified by doi:10.1126/science.1204062, please use {{cite journal}} (if it was published in a bona fide academic journal, otherwise {{cite report}} with
|doi=10.1126/science.1204062instead. - ^ "AstDys (21) Lutetia Ephemerides". Department of Mathematics, University of Pisa, Italy. Retrieved 2010-06-28.
- ^ a b Magri, C (1999). "Mainbelt Asteroids: Results of Arecibo and Goldstone Radar Observations of 37 Objects during 1980-1995". Icarus. 140 (2): 379. Bibcode:1999Icar..140..379M. doi:10.1006/icar.1999.6130.
- ^ a b c d e Amos, Jonathan (4 October 2010). "Asteroid Lutetia has thick blanket of debris". BBC News.
- ^ Lardner, Dionysius (1867). "The Planetoides". Handbook of astronomy. James Walton. p. 222. ISBN 1-4370-0602-7.
- ^ Goldschmidt, H. (June 1852). "Discovery of Lutetia Nov. 15". Monthly Notices of the Royal Astronomical Society. 12: 213. Bibcode:1852MNRAS..12..213G.
- ^ Leuschner, A. O. (1935). "Research surveys of the orbits and perturbations of minor planets 1 to 1091 from 1801.0 to 1929.5". Publications of Lick Observatory. 19: 29. Bibcode:1935PLicO..19....1L.
- ^ Pickering, Edward C. (January 1903). "Missing Asteroids". Harvard College Observatory Circular. 69: 7–8. Bibcode:1903HarCi..69....7P.
- ^ Attention: This template ({{cite doi}}) is deprecated. To cite the publication identified by doi:10.1051/0004-6361:20041505, please use {{cite journal}} (if it was published in a bona fide academic journal, otherwise {{cite report}} with
|doi=10.1051/0004-6361:20041505instead. - ^ Jim Baer (2008). "Recent Asteroid Mass Determinations". Personal Website. Retrieved 2008-11-28.
- ^ Birlan, M (2004). "Near-IR spectroscopy of asteroids 21 Lutetia, 89 Julia, 140 Siwa, 2181 Fogelin and 5480 (1989YK8) [sic], potential targets for the Rosetta mission; remote observations campaign on IRTF". New Astronomy. 9 (5): 343. arXiv:astro-ph/0312638. Bibcode:2004NewA....9..343B. doi:10.1016/j.newast.2003.12.005.
- ^ Lazzarin, M.; Marchi, S.; Magrin, S.; Barbieri, C. (2004). "Visible spectral properties of asteroid 21 Lutetia, target of Rosetta Mission" (PDF). Astronomy and Astrophysics. 425 (2): L25. Bibcode:2004A&A...425L..25L. doi:10.1051/0004-6361:200400054.
- ^ Feierberg, M; Witteborn, Fred C.; Lebofsky, Larry A. (1983). "Detection of silicate emission features in the 8- to 13 micrometre spectra of main belt asteroids". Icarus. 56 (3): 393. Bibcode:1983Icar...56..393F. doi:10.1016/0019-1035(83)90160-4.
- ^ Dollfus, A.; Geake, J. E. (1975). "Polarimetric properties of the lunar surface and its interpretation. VII – Other solar system objects". Proceedings of the 6th Lunar Science Conference, Houston, Texas, March 17–21. 3: 2749. Bibcode:1975LPSC....6.2749D.
- ^ "Lutetia: A rare survivor from the birth of Earth". ESO, Garching, Germany. November 14, 2011. Retrieved November 14, 2011.
- ^ Torppa, Johanna; Kaasalainen, Mikko; Michałowski, Tadeusz; Kwiatkowski, Tomasz; Kryszczyńska, Agnieszka; Denchev, Peter; Kowalski, Richard (2003). "Shapes and rotational properties of thirty asteroids from photometric data" (PDF). Icarus. 164 (2): 346. Bibcode:2003Icar..164..346T. doi:10.1016/S0019-1035(03)00146-5.
- ^ Attention: This template ({{cite doi}}) is deprecated. To cite the publication identified by doi:10.1051/0004-6361/201013994, please use {{cite journal}} (if it was published in a bona fide academic journal, otherwise {{cite report}} with
|doi=10.1051/0004-6361/201013994instead. - ^ Blue, Jennifer (1 March 2011). "Themes Approved for Asteroid (21) Lutetia'". USGS Astrogeology Science Center.
{{cite web}}: Italic or bold markup not allowed in:|publisher=(help)
External links
