3281 Maupertuis

Last updated • 3 min readFrom Wikipedia, The Free Encyclopedia

3281 Maupertuis
003281-asteroid shape model (3281) Maupertuis.png
Shape model of Maupertuis from its lightcurve
Discovery  [1]
Discovered by Y. Väisälä
Discovery site Turku Obs.
Discovery date24 February 1938
Designations
(3281) Maupertuis
Named after
 Pierre Louis Maupertuis   [1]
(French mathematician)
1938 DZ ·1961 TP
1970 AP ·1979 TV
main-belt   [1] [2]  ·(inner)
Vesta   [3]  · Flora   [4]
Orbital characteristics   [2]
Epoch 23 March 2018 (JD 2458200.5)
Uncertainty parameter 0
Observation arc 86.03 yr (31,422 d)
Aphelion 2.5798 AU
Perihelion 2.1203 AU
2.3501 AU
Eccentricity 0.0978
3.60 yr (1,316 d)
20.991°
0° 16m 24.96s / day
Inclination 5.9904°
348.46°
240.52°
Physical characteristics
Mean diameter
5.482±0.043  km [5]
5.680±0.031 km [6]
7.14 km (calculated) [4]
6.7295±0.0001  h [7] [lower-alpha 1]
6.72984±0.00001 h [8]
0.24(assumed) [4]
0.4611±0.0450 [6]
0.489±0.020 [5]
S (assumed) [4]
V (possibly)
12.7 [6]
12.9 [2] [4]
13.11±0.45 [9]

    3281 Maupertuis (prov. designation: 1938 DZ) is a bright Vesta asteroid from the inner regions of the asteroid belt. It was discovered on 24 February 1938, by Finnish astronomer Yrjö Väisälä at the Turku Observatory in southwest Finland. [1] The likely elongated V-type asteroid has a rotation period of 6.7 hours and measures approximately 5.5 kilometers (3.4 miles) in diameter. [4] It was named after French geodesist and mathematician Pierre Louis Maupertuis. [1]

    Contents

    Orbit and classification

    Maupertuis is a member of the Vesta family ( 401 ), [3] a giant asteroid family of typically bright V-type asteroids. Vestian asteroids have a composition akin to cumulate eucrites (HED meteorites) and are thought to have originated deep within 4 Vesta's crust, possibly from the Rheasilvia crater, a large impact crater on its southern hemisphere near the South pole, formed as a result of a sub-catastrophic collision. Vesta is the main belt's second-largest and second-most-massive body after Ceres. [10] [11] Based on osculating Keplerian orbital elements, the asteroid has also been classified as a member of the Flora family ( 402 ), a giant asteroid family and the largest family of stony asteroids in the main-belt. [4]

    It orbits the Sun in the inner asteroid belt at a distance of 2.1–2.6  AU once every 3 years and 7 months (1,316 days; semi-major axis of 2.35 AU). Its orbit has an eccentricity of 0.10 and an inclination of 6° with respect to the ecliptic. [2] The body's observation arc begins with a precovery taken at the Lowell Observatory in March 1931, or nearly 7 years prior to its official discovery observation at Turku. [1]

    Naming

    This minor planet was named after French geodesist and mathematician Pierre Louis Maupertuis (1698–1759), who was a member of the French Academy of Sciences and chief of the French Geodesic Mission to the Tornio river valley in Lapland, Finland, to conducted the degree measurement of the meridian (1736–1737), which determined that the Earth is oblate rather than prolate (see spheroid), as proposed by his rival Jacques Cassini. [1] The naming was published by the Minor Planet Center on 27 June 1991 ( M.P.C. 18451). [12] The lunar crater Maupertuis was also named in his honor.

    Physical characteristics

    Maupertuis is an assumed stony S-type asteroid. [4] Based on its high albedo (see below), and its membership to the Vesta family, it is possibly a V-type asteroid.

    Rotation period and poles

    In March 2010, a rotational lightcurve of Maupertuis was obtained from photometric observations by French amateur astronomer René Roy. Lightcurve analysis gave a well-defined rotation period of 6.7295 hours with an exceptionally high brightness amplitude of 1.22 magnitude ( U=3 ), indicative of a strongly elongated shape. [7] [lower-alpha 1]

    In March 2016, a second period was published based on data from the Lowell Photometric Database. Using lightcurve inversion and convex shape models, as well as distributed computing power and the help of individual volunteers, a sidereal period of 6.25033±0.00001 hours was derived from the database's sparse-in-time photometry data. Two spin axes at (62.0°, −66.0°) and (231.0°, −74.0°) in ecliptic coordinates (λ, β) were also determined. [8]

    Diameter and albedo

    According to the survey carried out by the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer, Maupertuis measures between 5.482 and 5.680 kilometers in diameter and its surface has an albedo between 0.4611 and 0.489. [5] [6] The Collaborative Asteroid Lightcurve Link assumes it to be a Florian asteroid and uses a lower albedo of 0.24 – derived from 8 Flora, the family's parent body – and consequently calculates a somewhat larger diameter of 7.14 kilometers based on an absolute magnitude of 12.9. [4]

    Notes

    1. 1 2 Polar luster diagram of (3281) Maupertuis (diagramme polaire de l'éclat). Summary figures for at the Asteroids and comets rotation curves, CdR, Raoul Behrend, Geneva Observatory.

    Related Research Articles

    <span class="mw-page-title-main">749 Malzovia</span>

    749 Malzovia is a stony background asteroid from the inner regions of the asteroid belt, approximately 11 kilometers in diameter. It was discovered on 5 April 1913, by Russian astronomer Sergey Belyavsky at the Simeiz Observatory on the Crimean peninsula. The elongated S-type asteroid has a rotation period of 5.9 hours. It was named after Russian amateur astronomer Nikolai Maltsov who founded the discovering Simeïs Observatory in 1900.

    956 Elisa is a Flora asteroid from the inner regions of the asteroid belt, approximately 10.5 kilometers in diameter. It was discovered on 8 August 1921, by German astronomer Karl Reinmuth at the Heidelberg Observatory. The V-type asteroid has a rotation period of 16.5 hours. It was named after Elisa Reinmuth, mother of the discoverer.

    1145 Robelmonte, provisional designation 1929 CC, is a Vestian asteroid from the inner regions of the asteroid belt, approximately 23 kilometers in diameter.

    2572 Annschnell, provisional designation 1950 DL, is a background asteroid from the inner regions of the asteroid belt, approximately 10 kilometers in diameter.

    5171 Augustesen, provisional designation 1987 SQ3, is a background asteroid and slow rotator from the inner regions of the asteroid belt, approximately 8 kilometers (5 miles) in diameter. It was discovered on 25 September 1987, by Danish astronomer Poul Jensen at the Brorfelde Observatory in Denmark. The suspected tumbler and presumed Vestian asteroid has an exceptionally slow rotation period of 480 hours and possibly an elongated shape. It was named after Danish astronomer Karl Augustesen.

    3268 De Sanctis, provisional designation 1981 DD, is a Vestian asteroid from the inner regions of the asteroid belt, approximately 6 kilometers in diameter. It was discovered on 26 February 1981, by European astronomers Henri Debehogne and Giovanni de Sanctis at ESO's La Silla Observatory in northern Chile. The asteroid was named after the second discoverer. The assumed S-type asteroid has a rotation period of 17 hours.

    <span class="mw-page-title-main">1251 Hedera</span>

    1251 Hedera is a background asteroid from the central regions of the asteroid belt, approximately 13 kilometers in diameter. It was discovered on 25 January 1933, by German astronomer Karl Reinmuth at the Heidelberg-Königstuhl State Observatory in southwest Germany. The asteroid was named for the climbing plant Hedera, commonly known as "ivy".

    1929 Kollaa, provisional designation 1939 BS, is a stony Vestian asteroid from the inner regions of the asteroid belt, approximately 7 kilometers in diameter. It was discovered by Finnish astronomer Yrjö Väisälä at Turku Observatory in Southwest Finland, on 20 January 1939. The asteroid was named after the Kollaa River in what is now Russia.

    4147 Lennon, provisional designation 1983 AY, is a stony Vestian asteroid and a potentially slow rotator from the inner regions of the asteroid belt, approximately 7 kilometers in diameter. It was discovered by American astronomer Brian Skiff at Lowell's Anderson Mesa Station on 12 January 1983. It was later named after musician John Lennon.

    <span class="mw-page-title-main">1459 Magnya</span>

    1459 Magnya, provisional designation 1937 VA, is a basaltic, slightly elongated asteroid from the outer regions of the asteroid belt, approximately 20 kilometers in diameter. Discovered by Grigory Neujmin at the Simeiz Observatory in 1937, this background asteroid was later named from the Latin word "Magnya", which means "clear, bright, wonderful" when literally translated into Russian. It is the only known basalt asteroid orbiting beyond 4 Vesta.

    <span class="mw-page-title-main">1841 Masaryk</span>

    1841 Masaryk (prov. designation: 1971 UO1) is a carbonaceous background asteroid from the outer region of the asteroid belt, approximately 46 kilometers in diameter. It was discovered on 26 October 1971, by Czech astronomer Luboš Kohoutek at Bergedorf Observatory in Hamburg, Germany. The asteroid was named after the first President of Czechoslovakia, Tomáš Garrigue Masaryk.

    4022 Nonna, provisional designation 1981 TL4, is a Vestian asteroid from the inner regions of the asteroid belt, approximately 4 kilometers (2.5 miles) kilometers in diameter. It was discovered on 8 October 1981, by Soviet–Russian astronomer Lyudmila Chernykh at the Crimean Astrophysical Observatory. The asteroid was named after Soviet actress Nonna Mordyukova. The nearly fast rotator has an exceptionally low lightcurve-amplitude indicating a nearly spherical shape.

    4003 Schumann, provisional designation 1964 ED, is a carbonaceous asteroid from the outer region of the asteroid belt, approximately 35 kilometers in diameter.

    4383 Suruga, provisional designation 1989 XP, is a Vestian asteroid and binary system from the inner regions of the asteroid belt, approximately 6.5 kilometers in diameter. It was discovered on 1 December 1989, by Japanese astronomer Yoshiaki Oshima at Gekko Observatory, Japan. The asteroid was named after the former Japanese Suruga Province. Its synchronous minor-planet moon, S/2013 (4383) 1, measures approximately 1.33 kilometers and has a period of 16.386 hours.

    2391 Tomita, provisional designation 1957 AA, is a Nysian asteroid from the inner regions of the asteroid belt, approximately 15 kilometers in diameter. The asteroid was discovered on 9 January 1957, by German astronomer Karl Reinmuth at Heidelberg Observatory in southern Germany. It was named after Japanese astronomer Kōichirō Tomita.

    <span class="mw-page-title-main">1496 Turku</span>

    1496 Turku, provisional designation 1938 SA1, is a Florian asteroid from the inner regions of the asteroid belt, approximately 8 kilometers in diameter. It was discovered on 22 September 1938, by astronomer Yrjö Väisälä at the Iso-Heikkilä Observatory in Turku, Finland. The asteroid was named for the Finnish city of Turku.

    17035 Velichko, provisional designation 1999 FC10, is a Vestian asteroid from the inner regions of the asteroid belt, approximately 4.5 kilometers in diameter.

    1535 Päijänne, provisional designation 1939 RC, is an asteroid from the outer region of the asteroid belt, approximately 25 kilometers in diameter. It was discovered on 9 September 1939, by Finnish astronomer Yrjö Väisälä at the Turku Observatory in Southwest Finland. It was later named for Lake Päijänne.

    2011 Veteraniya, provisional designation 1970 QB1, is a stony Vestian asteroid from the inner regions of the asteroid belt, approximately 6 kilometers in diameter. It was discovered on 30 August 1970, by Russian astronomer Tamara Smirnova at the Crimean Astrophysical Observatory, Nauchnyj, on the Crimean peninsula, and named for the Soviet veterans of the Second World War.

    13058 Alfredstevens, provisional designation 1990 WN3, is a stony Vestian asteroid from the inner regions of the asteroid belt, approximately 3 kilometers in diameter. It was discovered by Belgian astronomer Eric Elst at ESO's La Silla Observatory in Northern Chile, on 19 November 1990. The asteroid was named for Belgian painter Alfred Stevens.

    References

    1. 1 2 3 4 5 6 7 "3281 Maupertuis (1938 DZ)". Minor Planet Center. Retrieved 14 May 2018.
    2. 1 2 3 4 "JPL Small-Body Database Browser: 3281 Maupertuis (1938 DZ)" (2017-03-31 last obs.). Jet Propulsion Laboratory . Retrieved 14 May 2018.
    3. 1 2 "Asteroid 3281 Maupertuis – Nesvorny HCM Asteroid Families V3.0". Small Bodies Data Ferret. Retrieved 26 October 2019.
    4. 1 2 3 4 5 6 7 8 9 "LCDB Data for (3281) Maupertuis". Asteroid Lightcurve Database (LCDB). Retrieved 14 May 2018.
    5. 1 2 3 Masiero, Joseph R.; Grav, T.; Mainzer, A. K.; Nugent, C. R.; Bauer, J. M.; Stevenson, R.; et al. (August 2014). "Main-belt Asteroids with WISE/NEOWISE: Near-infrared Albedos". The Astrophysical Journal. 791 (2): 11. arXiv: 1406.6645 . Bibcode:2014ApJ...791..121M. doi:10.1088/0004-637X/791/2/121. S2CID   119293330.
    6. 1 2 3 4 Mainzer, A.; Grav, T.; Masiero, J.; Hand, E.; Bauer, J.; Tholen, D.; et al. (November 2011). "NEOWISE Studies of Spectrophotometrically Classified Asteroids: Preliminary Results". The Astrophysical Journal. 741 (2): 25. arXiv: 1109.6407 . Bibcode:2011ApJ...741...90M. doi:10.1088/0004-637X/741/2/90. S2CID   35447010. (catalog)
    7. 1 2 Behrend, Raoul. "Asteroids and comets rotation curves – (3281) Maupertuis". Geneva Observatory. Retrieved 14 May 2018.
    8. 1 2 Durech, J.; Hanus, J.; Oszkiewicz, D.; Vanco, R. (March 2016). "Asteroid models from the Lowell photometric database". Astronomy and Astrophysics. 587: 6. arXiv: 1601.02909 . Bibcode:2016A&A...587A..48D. doi:10.1051/0004-6361/201527573. S2CID   118427201.
    9. ↑ Veres, Peter; Jedicke, Robert; Fitzsimmons, Alan; Denneau, Larry; Granvik, Mikael; Bolin, Bryce; et al. (November 2015). "Absolute magnitudes and slope parameters for 250,000 asteroids observed by Pan-STARRS PS1 - Preliminary results". Icarus. 261: 34–47. arXiv: 1506.00762 . Bibcode:2015Icar..261...34V. doi:10.1016/j.icarus.2015.08.007. S2CID   53493339.
    10. ↑ Nesvorný, D.; Broz, M.; Carruba, V. (December 2014). "Identification and Dynamical Properties of Asteroid Families". Asteroids IV. pp. 297–321. arXiv: 1502.01628 . Bibcode:2015aste.book..297N. doi:10.2458/azu_uapress_9780816532131-ch016. ISBN   9780816532131. S2CID   119280014.
    11. ↑ Kelley, Michael S.; Vilas, Faith; Gaffey, Michael J.; Abell, Paul A. (September 2003). "Quantified mineralogical evidence for a common origin of 1929 Kollaa with 4 Vesta and the HED meteorites". Icarus. 165 (1): 215–218. Bibcode:2003Icar..165..215K. doi:10.1016/S0019-1035(03)00149-0.
    12. ↑ "MPC/MPO/MPS Archive". Minor Planet Center. Retrieved 14 May 2018.
    This page is based on this Wikipedia article
    Text is available under the CC BY-SA 4.0 license; additional terms may apply.
    Images, videos and audio are available under their respective licenses.