1020 Arcadia

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1020 Arcadia
Discovery [1]
Discovered by K. Reinmuth
Discovery site Heidelberg Obs.
Discovery date 7 March 1924
Designations
MPC designation (1020) Arcadia
Named after
Arcadia (Greek region)[2]
1924 QV · 1954 UA2
1975 EQ · 1977 QO2
main-belt[1][3] · (middle)
Agnia[4][5]
Orbital characteristics[3]
Epoch 23 March 2018 (JD 2458200.5)
Uncertainty parameter 0
Observation arc 93.89 yr (34,293 d)
Aphelion 2.9152 AU
Perihelion 2.6666 AU
2.7909 AU
Eccentricity 0.0445
4.66 yr (1,703 d)
18.189°
0° 12m 41.04s / day
Inclination 4.0598°
180.71°
37.691°
Physical characteristics
Mean diameter
10.067±0.090 km[6]
10.415±0.123 km[7]
13.02±0.49 km[8]
21.16 km (calculated)[9]
17.02±0.02 h[10]
0.057 (assumed)[9]
0.150±0.023[8]
0.2364±0.0456[7]
SMASS = S[3] · S[11]
S(SDSS-MFB)[9]
12.0[3] · 12.10[7][8][9]
12.29±0.11[11]

1020 Arcadia, provisional designation 1924 QV, is a stony Agnia asteroid from the central regions of the asteroid belt, approximately 11 kilometers (7 miles) in diameter. It was discovered on 7 March 1924, by German astronomer Karl Reinmuth at the Heidelberg Observatory in Heidelberg, Germany.[1] The asteroid was named after the Greek region of Arcadia.[2]

Orbit and classification[edit]

Arcadia is a member of the Agnia family (514),[4][5] a very large family of stony asteroids with more than 2000 known members.[12] They most likely formed from the breakup of a basalt object, which in turn was spawned from a larger parent body that underwent igneous differentiation.[5] The family's parent body and namesake is the asteroid 847 Agnia.[12]

It orbits the Sun in the central main-belt at a distance of 2.7–2.9 AU once every 4 years and 8 months (1,703 days; semi-major axis of 2.79 AU). Its orbit has an eccentricity of 0.04 and an inclination of 4° with respect to the ecliptic.[3] The body's observation arc begins at Heidelberg in March 1924, six days after its official discovery observation.[1]

Physical characteristics[edit]

In the SMASS classification, Arcadia is a common, stony S-type asteroid.[3] It has been characterized as an S-type by Pan-STARRS photometric survey,[11] as well as by SDSS-MFB (Masi Foglia Bus).[9]

Rotation period[edit]

In November 2011, a fragmentary rotational lightcurve of Arcadia was obtained from photometric observations by Gordon Gartrelle at the University of North Dakota. Lightcurve analysis gave a rotation period of 17.02 hours with a brightness amplitude of 0.05 magnitude (U=1).[10] As of 2018, no secure period has been obtained.[9]

Diameter and albedo[edit]

According to the survey carried out by the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer, Arcadia measures between 10.067 and 13.02 kilometers in diameter and its surface has an albedo between 0.150 and 0.2364.[6][7][8] The Collaborative Asteroid Lightcurve Link assumes an albedo 0.057, i.e. an albedo for a carbonaceous rather than for a stony asteroid, and consequently calculates a much larger diameter of 21.16 kilometers based on an absolute magnitude of 12.1.[9] It may be speculated whether this anomaly is a glitch in the data base.

Naming[edit]

This minor planet was named after named after the Greek region of Arcadia in central Peloponnese. It is also a celebrated mythological region, where the shepherd god Pan lived. The official naming citation was mentioned in The Names of the Minor Planets by Paul Herget in 1955 (H 97).[2]

References[edit]

  1. ^ a b c d "1020 Arcadia (1924 QV)". Minor Planet Center. Retrieved 8 March 2018. 
  2. ^ a b c Schmadel, Lutz D. (2007). Dictionary of Minor Planet Names – (1020) Arcadia. Springer Berlin Heidelberg. p. 88. ISBN 978-3-540-00238-3. Retrieved 8 March 2018. 
  3. ^ a b c d e f "JPL Small-Body Database Browser: 1020 Arcadia (1924 QV)" (2018-01-27 last obs.). Jet Propulsion Laboratory. Retrieved 8 March 2018. 
  4. ^ a b "Small Bodies Data Ferret". Nesvorny HCM Asteroid Families V3.0. Retrieved 8 March 2018. 
  5. ^ a b c Sunshine, Jessica M.; Bus, Schelte J.; McCoy, Timothy J.; Burbine, Thomas H.; Corrigan, Catherine M.; Binzel, Richard P. (August 2004). "High-calcium pyroxene as an indicator of igneous differentiation in asteroids and meteorites". Meteoritics and Planetary Science. 39 (8): 1343–1357. Bibcode:2004M&PS...39.1343S. doi:10.1111/j.1945-5100.2004.tb00950.x. Retrieved 8 March 2018. 
  6. ^ a b 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:1109.4096Freely accessible. Bibcode:2011ApJ...741...68M. doi:10.1088/0004-637X/741/2/68. Retrieved 8 March 2018. 
  7. ^ a b c d Mainzer, A.; Grav, T.; Masiero, J.; Hand, E.; Bauer, J.; Tholen, D.; et al. (November 2011). "NEOWISE Studies of Spectrophotometrically Classified Asteroids: Preliminary Results" (PDF). The Astrophysical Journal. 741 (2): 25. arXiv:1109.6407Freely accessible. Bibcode:2011ApJ...741...90M. doi:10.1088/0004-637X/741/2/90. Retrieved 8 March 2018. 
  8. ^ a b c d Masiero, Joseph R.; Mainzer, A. K.; Grav, T.; Bauer, J. M.; Cutri, R. M.; Nugent, C.; et al. (November 2012). "Preliminary Analysis of WISE/NEOWISE 3-Band Cryogenic and Post-cryogenic Observations of Main Belt Asteroids". The Astrophysical Journal Letters. 759 (1): 5. arXiv:1209.5794Freely accessible. Bibcode:2012ApJ...759L...8M. doi:10.1088/2041-8205/759/1/L8. Retrieved 8 March 2018. 
  9. ^ a b c d e f g "LCDB Data for (1020) Arcadia". Asteroid Lightcurve Database (LCDB). Retrieved 8 March 2018. 
  10. ^ a b Gartrelle, Gordon M. (April 2012). "Lightcurve Results for Eleven Asteroids". The Minor Planet Bulletin. 39 (2): 40–46. Bibcode:2012MPBu...39...40G. ISSN 1052-8091. Retrieved 8 March 2018. 
  11. ^ a b c 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:1506.00762Freely accessible. Bibcode:2015Icar..261...34V. doi:10.1016/j.icarus.2015.08.007. Retrieved 8 March 2018. 
  12. ^ a b Nesvorný, D.; Broz, M.; Carruba, V. (December 2014). "Identification and Dynamical Properties of Asteroid Families" (PDF). Asteroids IV: 297–321. arXiv:1502.01628Freely accessible. Bibcode:2015aste.book..297N. doi:10.2458/azu_uapress_9780816532131-ch016. Retrieved 8 March 2018. 

External links[edit]