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10241 Miličević, provisional designation 1999 AU6, is a carbonaceous Themistian asteroid from the outer regions of the asteroid belt, approximately 11 kilometers (6.8 miles) in diameter. It was discovered on 9 January 1999, by Croatian astronomer Korado Korlević at the Višnjan Observatory in Croatia. The C-type asteroid has a short rotation period of 3.87 hours and was named after hermit and amateur astronomer Don Nikola Miličević.[1][3]

10241 Miličević
Discovery [1]
Discovered byK. Korlević
Discovery siteVišnjan Obs.
Discovery date9 January 1999
Designations
MPC designation(10241) Miličević
Named after
Nikola Miličević[1]
(Croatian hermit)
1999 AU6 · 1981 UX24
1996 KB1 · 1997 WB49
main-belt[1][2] · (outer)[3]
Themis[4]
Orbital characteristics[2]
Epoch 23 March 2018 (JD 2458200.5)
Uncertainty parameter 0
Observation arc35.69 yr (13,034 d)
Aphelion3.5285 AU
Perihelion2.5672 AU
3.0479 AU
Eccentricity0.1577
5.32 yr (1,944 d)
345.06°
0° 11m 6.72s / day
Inclination1.6172°
151.77°
190.89°
Physical characteristics
Mean diameter
10.882±0.159 km[5][6]
8.39 km (calculated)[3]
3.87±0.03 h[7]
0.057 (assumed)[3]
0.065±0.005[5][6]
C[3][8]
13.4[6]
13.6[2]
13.66±0.11 (R)[7]
13.67±0.18[8]
14.11[3]

Contents

Orbit and classificationEdit

Miličević is a Themistian asteroid that belongs to the Themis family (602),[4] a very large family of carbonaceous asteroids, named after 24 Themis.[9] It orbits the Sun in the outer main-belt at a distance of 2.6–3.5 AU once every 5 years and 4 months (1,944 days; semi-major axis of 3.05 AU). Its orbit has an eccentricity of 0.16 and an inclination of 2° with respect to the ecliptic.[2]

The body's observation arc begins with its first observation at Palomar Observatory in October 1981, more than 17 years prior to its official discovery observation at Višnjan.[1]

Physical characteristicsEdit

Based on its classification to the Themis family and on observations conducted by the Pan-STARRS survey, Miličević is a carbonaceous C-type asteroid.[3][8]

Rotation periodEdit

In December 2014, a rotational lightcurve of Miličević was obtained from photometric observations in the R-band by astronomers at the Palomar Transient Factory in California. Lightcurve analysis gave a short rotation period of 3.87 hours with a brightness amplitude of 0.34 magnitude (U=2).[3][7]

Diameter and albedoEdit

According to the survey carried out by the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer, Miličević measures 10.882 kilometers in diameter and its surface has an albedo of 0.065,[5][6] while the Collaborative Asteroid Lightcurve Link assumes a standard albedo for a carbonaceous asteroid of 0.057 and calculates a diameter of 8.39 kilometers based on an absolute magnitude of 14.11.[3]

NamingEdit

This minor planet was named after Don Nikola Miličević (1887-1963), Croatian amateur astronomer and last administrator of Blaca hermitage. The Hermitage is an UNESCO World Heritage Site located on the Brač island in Croatia.[1] The official naming citation was published by the Minor Planet Center on 15 December 2005 (M.P.C. 55720).[10]

ReferencesEdit

  1. ^ a b c d e f "10241 Milicevic (1999 AU6)". Minor Planet Center. Retrieved 30 April 2018.
  2. ^ a b c d "JPL Small-Body Database Browser: 10241 Milicevic (1999 AU6)" (2017-07-02 last obs.). Jet Propulsion Laboratory. Retrieved 30 April 2018.
  3. ^ a b c d e f g h i "LCDB Data for (10241) Miličević". Asteroid Lightcurve Database (LCDB). Retrieved 30 April 2018.
  4. ^ a b "Small Bodies Data Ferret". Nesvorny HCM Asteroid Families V3.0. Retrieved 30 April 2018.
  5. ^ a b c 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. Retrieved 30 April 2018.
  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. arXiv:1109.6407. Bibcode:2011ApJ...741...90M. doi:10.1088/0004-637X/741/2/90. Retrieved 30 April 2018.
  7. ^ a b c Chang, Chan-Kao; Lin, Hsing-Wen; Ip, Wing-Huen; Prince, Thomas A.; Kulkarni, Shrinivas R.; Levitan, David; et al. (December 2016). "Large Super-fast Rotator Hunting Using the Intermediate Palomar Transient Factory". The Astrophysical Journal Supplement Series. 227 (2): 13. arXiv:1608.07910. Bibcode:2016ApJS..227...20C. doi:10.3847/0067-0049/227/2/20. Retrieved 30 April 2018.
  8. ^ 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" (PDF). Icarus. 261: 34–47. arXiv:1506.00762. Bibcode:2015Icar..261...34V. doi:10.1016/j.icarus.2015.08.007. Retrieved 30 April 2018.
  9. ^ Nesvorný, D.; Broz, M.; Carruba, V. (December 2014). "Identification and Dynamical Properties of Asteroid Families" (PDF). Asteroids IV: 297–321. arXiv:1502.01628. Bibcode:2015aste.book..297N. doi:10.2458/azu_uapress_9780816532131-ch016. Retrieved 30 April 2018.
  10. ^ "MPC/MPO/MPS Archive". Minor Planet Center. Retrieved 30 April 2018.

External linksEdit