4349 Tibúrcio

4349 Tibúrcio
Discovery [1]
Discovered by W. Landgraf
Discovery site La Silla Obs.
Discovery date 5 June 1989
Designations
MPC designation 4349 Tiburcio
Named after
 Júlio Tibúrcio
(amateur astronomer)[2]
1989 LX · 1931 AE
1951 YV1 · 1959 SS
1968 WD · 1982 BJ4
1984 MJ · 1986 AZ2
main-belt · (middle) [3]
Orbital characteristics [1]
Epoch 31 July 2016 (JD 2457600.5)
Uncertainty parameter 0
Observation arc 85.39 yr (31,188 days)    
Aphelion 3.2537 AU
Perihelion 1.9881 AU
2.6209 AU
Eccentricity 0.2415
4.24 yr (1,550 days)
138.20°
0° 13m 56.28s / day
Inclination 10.731°
90.477°
280.49°
Physical characteristics
Dimensions 24.91±0.28 km[4]
26.12 km (derived)[3]
26.14±1.8 km (IRAS:4)[1]
26.45±10.54 km[5]
28.091±0.371 km[6]
16.284±0.003 h[lower-alpha 1]
0.0345±0.0053[6]
0.040±0.041[5]
0.0493 (derived)[3]
0.0540±0.008 (IRAS:4)[1]
0.061±0.002[4]
X [7] · S [3]
11.7[4][6]
11.8[1][3]
11.94±0.44[7]
12.00[5]

    4349 Tibúrcio, provisional designation 1989 LX, is a dark asteroid from the middle region of the asteroid belt, approximately 26 kilometers in diameter. It was discovered by German astronomer Werner Landgraf at ESO's La Silla Observatory in northern Chile, on 5 June 1989.[8] With 53.5°, it had been the asteroid with the smallest angular distance from the Sun ever discovered.[9]:395

    The asteroid is classified as both, a stony S-type body by the Collaborative Asteroid Lightcurve Link (CALL) and as a X-type asteroid by Pan-STARRS' large-scale survey. It orbits the Sun at a distance of 2.0–3.3 AU once every 4 years and 3 months (1,550 days). Its orbit has an eccentricity of 0.24 and an inclination of 11° with respect to the ecliptic.[1] The first precovery was taken at the U.S. Lowell Observatory in 1931, extending the asteroid's observation arc by 58 years prior to its discovery.[8]

    A rotational light-curve for this asteroid was obtained from photometric observations by astronomer David Higgins at the Australian Hunters Hill Observatory in October 2010. The light-curve gave a well-defined rotation period of 16.284±0.003 hours with a brightness variation of 0.40 in magnitude (U=3).[lower-alpha 1]

    According to the space-based surveys carried out by the Infrared Astronomical Satellite IRAS, the Japanese Akari satellite, and NASA's Wide-field Infrared Survey Explorer with its NEOWISE mission, the asteroid measures between 24.9 and 28.1 kilometers in diameter, and its surface has a low albedo between 0.034 and 0.061.[1][4][5][6] while CALL assumes an albedo of 0.049 and calculates a diameter of 26.1 kilometers, based on an absolute magnitude of 11.8.[3]

    The minor planet was named after Brazilian amateur astronomer and student of information science, Júlio César dos Santos Tibúrcio.[2] Naming citation was published on 8 June 1990 (M.P.C. 16445).[10]

    References

    1. 1 2 Higgins (2011) web: rotation period 16.284±0.003 hours with a brightness amplitude of 0.40 mag. Quality Code: U=3 (Denotes a secure result within the precision given and no ambiguity.). Summary figures at Collaborative Asteroid Lightcurve Link (CALL) for (4349) Tiburcio
    1. 1 2 3 4 5 6 7 "JPL Small-Body Database Browser: 4349 Tiburcio (1989 LX)" (2016-05-31 last obs.). Jet Propulsion Laboratory. Retrieved 3 August 2016.
    2. 1 2 Schmadel, Lutz D. (2007). Dictionary of Minor Planet Names – (4349) Tibúrcio. Springer Berlin Heidelberg. p. 373. ISBN 978-3-540-00238-3. Retrieved 3 August 2016.
    3. 1 2 3 4 5 6 "LCDB Data for (4349) Tiburcio". Asteroid Lightcurve Database (LCDB). Retrieved 3 August 2016.
    4. 1 2 3 4 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. Retrieved 3 August 2016.
    5. 1 2 3 4 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 3 August 2016.
    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:1109.6407Freely accessible. Bibcode:2011ApJ...741...90M. doi:10.1088/0004-637X/741/2/90. Retrieved 3 August 2016.
    7. 1 2 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 3 August 2016.
    8. 1 2 "4349 Tiburcio (1989 LX)". Minor Planet Center. Retrieved 3 August 2016.
    9. ↑ Marsden, B. G. (December 1993). "Asteroid and Comet Surveys". Astronomy from wide-field imaging: proceedings of the 161st Symposium of the International Astronomical Union: 385. Bibcode:1994IAUS..161..385M. Retrieved 3 January 2016.
    10. ↑ "MPC/MPO/MPS Archive". Minor Planet Center. Retrieved 3 August 2016.

    External links

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