4354 Euclides

4354 Euclides /juːˈklaɪdiːz/, provisional designation 2142 P-L, is a dark Dorian asteroid from the central regions of the asteroid belt, approximately 12 kilometers (7 miles) in diameter. It was discovered on 24 September 1960, by Dutch astronomer couple Ingrid and Cornelis van Houten on photographic plates taken by Dutch–American astronomer Tom Gehrels at Palomar Observatory in California. The likely C-type asteroid was named after the Greek mathematician Euclid.[1]

4354 Euclides
Discovery [1]
Discovered byC. J. van Houten
I. van Houten-G.
T. Gehrels
Discovery sitePalomar Obs.
Discovery date24 September 1960
Designations
(4354) Euclides
Pronunciation/juːˈklaɪdiːz/[2]
Named after
Euclid (Εὐκλείδης Eukleidēs)[1]
(Greek mathematician)
2142 P-L · 1971 BL2
1979 YO6 · 1983 RF
main-belt [1][3] · (middle)
Dora [4]
Orbital characteristics [3]
Epoch 23 March 2018 (JD 2458200.5)
Uncertainty parameter 0
Observation arc63.66 yr (23,250 d)
Aphelion3.3787 AU
Perihelion2.2128 AU
2.7957 AU
Eccentricity0.2085
4.67 yr (1,707 d)
62.073°
0° 12m 38.88s / day
Inclination7.4252°
192.98°
242.62°
Physical characteristics
Mean diameter
12.339±0.282 km[5]
0.051±0.005[5]
C (est. Dora family)
13.5[1][3]

    Orbit and classification

    Euclides is a core member of the Dora family (512),[4] a well-established central asteroid family of more than 1,200 carbonaceous asteroids. The family's namesake is 668 Dora. It is alternatively known as the "Zhongolovich family", named after its presumably largest member 1734 Zhongolovich. The Dora family may also contain a subfamily.[6][7]:13,23

    It orbits the Sun in the central asteroid belt at a distance of 2.2–3.4 AU once every 4 years and 8 months (1,707 days; semi-major axis of 2.8 AU). Its orbit has an eccentricity of 0.21 and an inclination of 7° with respect to the ecliptic.[3] The body's observation arc begins with a precovery taken at Palomar in July 1954, or six years prior to its official discovery observation.[1]

    Palomar–Leiden survey

    The survey designation "P-L" stands for Palomar–Leiden, named after Palomar Observatory and Leiden Observatory, which collaborated on the fruitful Palomar–Leiden survey in the 1960s. Gehrels used Palomar's Samuel Oschin telescope (also known as the 48-inch Schmidt Telescope), and shipped the photographic plates to Ingrid and Cornelis van Houten at Leiden Observatory where astrometry was carried out. The trio are credited with the discovery of several thousand asteroid discoveries.[8]

    Physical characteristics

    Although the asteroids spectral type has not been determined, it is likely a common, carbonaceous C-type asteroid, as Euclides belongs to the Dora family.[4] As of 2018, no rotational lightcurve of Euclides has been obtained from photometric observations. The body's rotation period, pole and shape remain unknown.[3]

    Diameter and albedo

    According to the survey carried out by the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer, Euclides measures 12.339 kilometers in diameter and its surface has an albedo of 0.051, typical for a carbonaceous asteroid.[5]

    Naming

    This minor planet was named after the Greek mathematician and Euclid (also: Euclides, or Eukleides). The "father of geometry" lived in Alexandria about 300 B.C.[1] The official naming citation was published by the Minor Planet Center on 8 July 1990 (M.P.C. 16594).[9] The lunar crater Euclides was also named in his honor.

    References
    1. "4354 Euclides (2142 P-L)". Minor Planet Center. Retrieved 27 May 2018.
    2. Noah Webster (1884) A Practical Dictionary of the English Language
    3. "JPL Small-Body Database Browser: 4354 Euclides (2142 P-L)" (2018-02-26 last obs.). Jet Propulsion Laboratory. Retrieved 27 May 2018.
    4. "Asteroid 4354 Euclides". Small Bodies Data Ferret. Retrieved 27 May 2018.
    5. Masiero, Joseph R.; Mainzer, A. K.; Grav, T.; Bauer, J. M.; Cutri, R. M.; Dailey, J.; et al. (November 2011). "Main Belt Asteroids with WISE/NEOWISE. I. Preliminary Albedos and Diameters". The Astrophysical Journal. 741 (2): 20. arXiv:1109.4096. Bibcode:2011ApJ...741...68M. doi:10.1088/0004-637X/741/2/68.
    6. Broz, M.; Morbidelli, A.; Bottke, W. F.; Rozehnal, J.; Vokrouhlický, D.; Nesvorný, D. (March 2013). "Constraining the cometary flux through the asteroid belt during the late heavy bombardment". Astronomy and Astrophysics. 551: 16. arXiv:1301.6221. Bibcode:2013A&A...551A.117B. doi:10.1051/0004-6361/201219296.
    7. 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.
    8. "Minor Planet Discoverers". Minor Planet Center. 2018. Retrieved 27 May 2018.
    9. "MPC/MPO/MPS Archive". Minor Planet Center. Retrieved 27 May 2018.

    This article is issued from Wikipedia. The text is licensed under Creative Commons - Attribution - Sharealike. Additional terms may apply for the media files.