487 Venetia

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487 Venetia
Discovery [1]
Discovered by L. Carnera
Discovery site Heidelberg Obs.
Discovery date 9 July 1902
Designations
MPC designation (487) Venetia
Named after
Veneto (Italian region)[2]
1902 JL
main-belt · (middle)[3]
Orbital characteristics[1]
Epoch 16 February 2017 (JD 2457800.5)
Uncertainty parameter 0
Observation arc 114.63 yr (41,868 days)
Aphelion 2.9063 AU
Perihelion 2.4333 AU
2.6698 AU
Eccentricity 0.0886
4.36 yr (1,593 days)
8.3676°
0° 13m 33.24s / day
Inclination 10.245°
114.82°
280.52°
Physical characteristics
Dimensions 59.046±0.458 km[4]
63.15±1.3 km (IRAS:22)[5]
65.562±0.795 km[6]
66.13±0.84 km[7]
10.62±0.02 h[8]
12.73 h[9]
13.28 h[10]
13.33170 h[11]
13.34±0.01 h[3][12]
13.34153 h[13]
13.342±0.002 h[14]
18 h (dated)[15]
0.2284±0.0421[6]
0.239±0.008[7]
0.2457±0.011 (IRAS:22)[5]
0.328±0.043[4]
B–V = 0.852[1]
U–B = 0.424[1]
Tholen = S[1] · K[16] · S[3]
8.14[1][3][5][6][7]

487 Venetia, provisional designation 1902 JL, is a rare-type stony asteroid from the middle regions of the asteroid belt, approximately 63 kilometers in diameter. It was discovered on 9 July 1902, by Italian astronomer Luigi Carnera at Heidelberg Observatory in southwest Germany.[17] It was later named for the Italian Veneto region where the city of Venice is located.[2]

Orbit and classification[edit]

Venetia orbits the Sun in the middle main-belt at a distance of 2.4–2.9 AU once every 4 years and 4 months (1,593 days). Its orbit has an eccentricity of 0.09 and an inclination of 10° with respect to the ecliptic.[1] The body's observation arc begins in 1913, at the Collegio Romano Observatory (531) in Italy, approximately 17 months after its official discovery observation at Heidelberg.[17]

Physical characteristics[edit]

On the taxonomic scheme, Venetia is a common, featureless S-type asteroid.[1] More recently, polarimetric observations refined its classification to a rare K-type asteroid.[16]

Rotation period[edit]

In March 2014, the so-far best rated rotational lightcurve was obtained by Italian astronomer Andrea Ferrero at the Bigmuskie Observatory (B88) in Mombercelli, Italy. It gave a well-defined rotation period of 13.34 hours with a brightness variation of 0.20 magnitude (U=3).[3][12] The result supersedes previously measured periods of 10.62 to 18 hours.[8][9][10][15]

Spin axis[edit]

In two separate studies, groups of German, Russian and Swedish astronomers also modeled Venetia's lightcurve from various data sources in 2000 and 2002. They found a spin axis of (259.0°, −30.0°) and (268.0°, −24.0°) in ecliptic coordinates (λ, β), as well as a concurring rotation period of 13.33170 and 13.34153 hours, respectively (U=n.a.).[11][13]

Diameter and albedo[edit]

According to the surveys carried out by the Infrared Astronomical Satellite IRAS, the Japanese Akari satellite, and NASA's Wide-field Infrared Survey Explorer with its subsequent NEOWISE mission, Venetia measures between 59.046 and 66.13 kilometers in diameter and its surface has an albedo between 0.228 and 0.328.[4][5][6][7] The Collaborative Asteroid Lightcurve Link adopts the results obtained by IRAS, that is, an albedo of 0.2457 and a diameter of 63.15 kilometers with an absolute magnitude of 8.14.[3]

Naming[edit]

This minor planet was named for the region of Veneto with its capital and largest city Venice. The region is located in northeast Italy between the Po River and the Alps. Naming was proposed by Italian astronomer Elia Millosevich.[2]

Naming citation was first mentioned in The Names of the Minor Planets by Paul Herget in 1955 (H 52) and amended by Lutz Schmadel for the Dictionary of Minor Planet Names based on a private communication with astronomer Piero Sicoli.[2]

References[edit]

  1. ^ a b c d e f g h "JPL Small-Body Database Browser: 487 Venetia (1902 JL)" (2017-02-23 last obs.). Jet Propulsion Laboratory. Retrieved 7 April 2017. 
  2. ^ a b c d Schmadel, Lutz D. (2007). Dictionary of Minor Planet Names – (487) Venetia. Springer Berlin Heidelberg. p. 53. ISBN 978-3-540-00238-3. Retrieved 7 April 2017. 
  3. ^ a b c d e f "LCDB Data for (487) Venetia". Asteroid Lightcurve Database (LCDB). Retrieved 7 April 2017. 
  4. ^ a b c 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. Bibcode:2014ApJ...791..121M. arXiv:1406.6645Freely accessible. doi:10.1088/0004-637X/791/2/121. Retrieved 7 April 2017. 
  5. ^ a b c d Tedesco, E. F.; Noah, P. V.; Noah, M.; Price, S. D. (October 2004). "IRAS Minor Planet Survey V6.0". NASA Planetary Data System. Bibcode:2004PDSS...12.....T. Retrieved 7 April 2017. 
  6. ^ 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. Bibcode:2011ApJ...741...90M. arXiv:1109.6407Freely accessible. doi:10.1088/0004-637X/741/2/90. Retrieved 7 April 2017. 
  7. ^ a b c d Usui, Fumihiko; Kuroda, Daisuke; Müller, Thomas G.; Hasegawa, Sunao; Ishiguro, Masateru; Ootsubo, Takafumi; et al. (October 2011). "Asteroid Catalog Using Akari: AKARI/IRC Mid-Infrared Asteroid Survey" (PDF). Publications of the Astronomical Society of Japan. 63 (5): 1117–1138. Bibcode:2011PASJ...63.1117U. doi:10.1093/pasj/63.5.1117. Retrieved 7 April 2017. 
  8. ^ a b Behrend, Raoul. "Asteroids and comets rotation curves – (487) Venetia". Geneva Observatory. Retrieved 7 April 2017. 
  9. ^ a b Neely, A. W. (December 1992). "CCD Photometry of Asteroid 487 Venetia". The Minor Planet Bulletin. 19.: 31. Bibcode:1992MPBu...19...31N. Retrieved 7 April 2017. 
  10. ^ a b Schober, H. J.; Erikson, A.; Hahn, G.; Lagerkvist, C.-I.; Albrecht, R.; Ornig, W.; et al. (June 1994). "Physical studies of asteroids. XXVIII. Lightcurves and photoelectric photometry of asteroids 2, 14, 51, 105, 181, 238, 258, 369, 377, 416, 487, 626, 679, 1048 and 2183". Astronomy and Astrophysics Supplement Series. 105. Bibcode:1994A&AS..105..281S. Retrieved 7 April 2017. 
  11. ^ a b Tungalag, N.; Shevchenko, V. G.; Lupishko, D. F. (December 2002). "Rotation parameters and shapes of 15 asteroids". Kinematika I Fizika Nebesnykh Tel: 508–516. Bibcode:2002KFNT...18..508T. Retrieved 7 April 2017. 
  12. ^ a b Ferrero, Andrea (July 2014). "Period Determination of Six Main Belt Asteroids". The Minor Planet Bulletin. 41 (3): 184–185. Bibcode:2014MPBu...41..184F. ISSN 1052-8091. Retrieved 7 April 2017. 
  13. ^ a b Erikson, A.; Mottola, S.; Lagerros, J. S. V.; Lindgren, M.; Piironen, J.; Oja, T.; et al. (October 2000). "The Near-Earth Objects Follow-up Program. III. 32 Lightcurves for 12 Objects from 1992 and 1995". Icarus. 147 (2): 487–497. Bibcode:2000Icar..147..487E. doi:10.1006/icar.2000.6457. Retrieved 7 April 2017. 
  14. ^ Marciniak, A.; Pilcher, F.; Oszkiewicz, D.; Santana-Ros, T.; Urakawa, S.; Fauvaud, S.; et al. (December 2015). "Against the biases in spins and shapes of asteroids". Planetary and Space Science. 118: 256–266. Bibcode:2015P&SS..118..256M. doi:10.1016/j.pss.2015.06.002. Retrieved 7 April 2017. 
  15. ^ a b Weidenschilling, S. J.; Chapman, C. R.; Davis, D. R.; Greenberg, R.; Levy, D. H. (August 1990). "Photometric geodesy of main-belt asteroids. III - Additional lightcurves". Icarus: 402–447. Bibcode:1990Icar...86..402W. ISSN 0019-1035. doi:10.1016/0019-1035(90)90227-Z. Retrieved 7 April 2017. 
  16. ^ a b Belskaya, I. N.; Fornasier, S.; Tozzi, G. P.; Gil-Hutton, R.; Cellino, A.; Antonyuk, K.; et al. (March 2017). "Refining the asteroid taxonomy by polarimetric observations". Icarus. 284: 30–42. Bibcode:2017Icar..284...30B. doi:10.1016/j.icarus.2016.11.003. Retrieved 7 April 2017. 
  17. ^ a b "487 Venetia (1902 JL)". Minor Planet Center. Retrieved 7 April 2017. 

External links[edit]