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1576 Fabiola

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1576 Fabiola
Shape model of Fabiola from its lightcurve
Discovery[1]
Discovered byS. Arend
Discovery siteUccle Obs.
Discovery date30 September 1948
Designations
(1576) Fabiola
Named after
Queen Fabiola of Belgium[2]
1948 SA · 1931 RV
1931 TQ2 · 1933 BZ
1939 CS · 1943 YA
1948 TU1 · 1948 UJ
1950 DZ
main-belt · (outer)
Themis[3][4]
Orbital characteristics[1]
Epoch 4 September 2017 (JD 2458000.5)
Uncertainty parameter 0
Observation arc85.66 yr (31,288 days)
Aphelion3.6746 AU
Perihelion2.6257 AU
3.1501 AU
Eccentricity0.1665
5.59 yr (2,042 days)
130.30°
0° 10m 34.68s / day
Inclination0.9514°
166.62°
244.20°
Physical characteristics
Dimensions21.33±8.66 km[5]
23.49±0.43 km[6]
26.22±1.79 km[7]
27.25±1.7 km[8]
27.357±0.240 km[9]
28.6±2.9 km[10]
30±3 km[11]
30.150±0.400 km[12]
6.7 h[13]
0.0746±0.0139[12]
0.08±0.02[11][10]
0.0913±0.013[8]
0.100±0.015[7]
0.11±0.09[5]
0.115±0.015[9]
0.123±0.018[6]
Tholen = BU[1][3]
B–V = 0.632[1]
U–B = 0.405[1]
11.04[1][3][6][7][8][10][11][12] · 11.13[5] · 11.17±0.17[14]

1576 Fabiola, provisional designation 1948 SA, is a Themistian asteroid from the outer regions of the asteroid belt, approximately 27 kilometers in diameter. It was discovered on 30 September 1948, by Belgian astronomer Sylvain Arend at the Royal Observatory of Belgium in Uccle.[15] The asteroid was named after Queen Fabiola of Belgium.[2]

Orbit and classification

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Fabiola is a Themistian asteroid that belongs to the Themis family (602), a very large family of carbonaceous asteroids, named after 24 Themis.[3][4][16] It orbits the Sun in the outer main-belt at a distance of 2.6–3.7 AU once every 5 years and 7 months (2,042 days). Its orbit has an eccentricity of 0.17 and an inclination of 1° with respect to the ecliptic.[1]

The asteroid was first identified as 1931 RV at Simeiz Observatory in September 1931. The body's observation arc begins with its identification as 1931 TQ2 at Lowell Observatory in October 1931, almost 17 years prior to its official discovery observation at Uccle.[15]

Physical characteristics

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In the Tholen classification, Fabiola has an ambiguous spectral type, similar to the B-type asteroids ("bright" carbonaceous asteroids), yet with an "unusual" spectra (BU).[1]

Rotation period

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In November 1976, a rotational lightcurve of Fabiola was obtained from photometric observations by Swedish astronomer Claes-Ingvar Lagerkvist at Uppsala Observatory. Lightcurve analysis gave a rotation period of 6.7 hours with a brightness amplitude of 0.2 magnitude (U=2).[13]

Diameter and albedo

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According to the surveys carried out by the Infrared Astronomical Satellite IRAS, the Japanese Akari satellite and the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer, Fabiola measures between 21.33 and 30.150 kilometers in diameter and its surface has an albedo between 0.0746 and 0.123.[5][6][7][8][9][10][11][12]

The Collaborative Asteroid Lightcurve Link adopts the results obtained by IRAS, that is, an albedo of 0.0913 and a diameter of 27.25 kilometers based on an absolute magnitude of 11.04.[3][8]

Naming

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This minor planet was named after Queen Fabiola of Belgium (1928–2014).[2] The official naming citation was published by the Minor Planet Center on 31 January 1962 (M.P.C. 2116).[17]

References

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  1. ^ a b c d e f g h "JPL Small-Body Database Browser: 1576 Fabiola (1948 SA)" (2017-06-05 last obs.). Jet Propulsion Laboratory. Retrieved 6 September 2017.
  2. ^ a b c Schmadel, Lutz D. (2007). "(1576) Fabiola". Dictionary of Minor Planet Names. Springer Berlin Heidelberg. p. 125. doi:10.1007/978-3-540-29925-7_1577. ISBN 978-3-540-00238-3.
  3. ^ a b c d e "LCDB Data for (1576) Fabiola". Asteroid Lightcurve Database (LCDB). Retrieved 6 September 2017.
  4. ^ a b "Asteroid 1576 Fabiola – Nesvorny HCM Asteroid Families V3.0". Small Bodies Data Ferret. Retrieved 26 October 2019.
  5. ^ a b c d Nugent, C. R.; Mainzer, A.; Bauer, J.; Cutri, R. M.; Kramer, E. A.; Grav, T.; et al. (September 2016). "NEOWISE Reactivation Mission Year Two: Asteroid Diameters and Albedos". The Astronomical Journal. 152 (3): 12. arXiv:1606.08923. Bibcode:2016AJ....152...63N. doi:10.3847/0004-6256/152/3/63.
  6. ^ 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:1209.5794. Bibcode:2012ApJ...759L...8M. doi:10.1088/2041-8205/759/1/L8. Retrieved 6 September 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". Publications of the Astronomical Society of Japan. 63 (5): 1117–1138. Bibcode:2011PASJ...63.1117U. doi:10.1093/pasj/63.5.1117. (online, AcuA catalog p. 153)
  8. ^ a b c d e Tedesco, E. F.; Noah, P. V.; Noah, M.; Price, S. D. (October 2004). "IRAS Minor Planet Survey V6.0". NASA Planetary Data System. 12: IRAS-A-FPA-3-RDR-IMPS-V6.0. Bibcode:2004PDSS...12.....T. Retrieved 22 October 2019.
  9. ^ 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. arXiv:1406.6645. Bibcode:2014ApJ...791..121M. doi:10.1088/0004-637X/791/2/121. Retrieved 6 September 2017.
  10. ^ a b c d Alí-Lagoa, V.; Licandro, J.; Gil-Hutton, R.; Cañ; ada-Assandri, M.; Delbo', M.; et al. (June 2016). "Differences between the Pallas collisional family and similarly sized B-type asteroids". Astronomy and Astrophysics. 591: 11. Bibcode:2016A&A...591A..14A. doi:10.1051/0004-6361/201527660. hdl:11336/63614.
  11. ^ a b c d Alí-Lagoa, V.; de León, J.; Licandro, J.; Delbó, M.; Campins, H.; Pinilla-Alonso, N.; et al. (June 2013). "Physical properties of B-type asteroids from WISE data". Astronomy and Astrophysics. 554: 16. arXiv:1303.5487. Bibcode:2013A&A...554A..71A. doi:10.1051/0004-6361/201220680. Retrieved 6 September 2017.
  12. ^ 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". The Astrophysical Journal. 741 (2): 25. arXiv:1109.6407. Bibcode:2011ApJ...741...90M. doi:10.1088/0004-637X/741/2/90.
  13. ^ a b Lagerkvist, C.-I. (March 1978). "Photographic photometry of 110 main-belt asteroids". Astronomy and Astrophysics Supplement Series. 31: 361–381. Bibcode:1978A&AS...31..361L. Retrieved 6 September 2017.
  14. ^ 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. Retrieved 6 September 2017.
  15. ^ a b "1576 Fabiola (1948 SA)". Minor Planet Center. Retrieved 6 September 2017.
  16. ^ 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.
  17. ^ Schmadel, Lutz D. (2009). "Appendix – Publication Dates of the MPCs". Dictionary of Minor Planet Names – Addendum to Fifth Edition (2006–2008). Springer Berlin Heidelberg. p. 221. doi:10.1007/978-3-642-01965-4. ISBN 978-3-642-01964-7.
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