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10241 Miličević

From Wikipedia, the free encyclopedia
Themistian asteroid

10241 Miličević
Discovery[1]
Discovered byK. Korlević
Discovery siteVišnjan Obs.
Discovery date9 January 1999
Designations
(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 arc35.69yr (13,034 d)
Aphelion3.5285AU
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
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]

10241 Miličević, provisional designation1999 AU6, is a carbonaceous Themistianasteroid from the outer regions of theasteroid belt, approximately 11 kilometers (6.8 miles) in diameter. It was discovered on 9 January 1999, by Croatian astronomerKorado Korlević at theVišnjan Observatory in Croatia. TheC-type asteroid has a shortrotation period of 3.87 hours and was named afterhermit and amateur astronomer DonNikola Miličević.[1][3]

Orbit and classification

[edit]

Miličević is a Themistian asteroid that belongs to theThemis family (602),[4] a very largefamily of carbonaceous asteroids, named after24 Themis.[9] It orbits the Sun in theouter 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 aneccentricity of 0.16 and aninclination of 2° with respect to theecliptic.[2]

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

Physical characteristics

[edit]

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

Rotation period

[edit]

In December 2014, a rotationallightcurve ofMiličević was obtained fromphotometric observations in the R-band by astronomers at thePalomar Transient Factory in California. Lightcurve analysis gave a shortrotation period of 3.87 hours with a brightness amplitude of 0.34magnitude (U=2).[3][7]

Diameter and albedo

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

Naming

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Thisminor planet was named after DonNikola Miličević (1887–1963), Croatian amateur astronomer and last administrator ofBlaca hermitage. TheHermitage is a UNESCOWorld Heritage Site located on theBrač island in Croatia.[1] The official naming citation was published by theMinor Planet Center on 15 December 2005 (M.P.C. 55720).[10]

References

[edit]
  1. ^abcdef"10241 Milicevic (1999 AU6)".Minor Planet Center. Retrieved30 April 2018.
  2. ^abcd"JPL Small-Body Database Browser: 10241 Milicevic (1999 AU6)" (2017-07-02 last obs.).Jet Propulsion Laboratory. Retrieved30 April 2018.
  3. ^abcdefghi"LCDB Data for (10241) Miličević". Asteroid Lightcurve Database (LCDB). Retrieved30 April 2018.
  4. ^ab"Asteroid 10241 Milicevic – Nesvorny HCM Asteroid Families V3.0".Small Bodies Data Ferret. Retrieved27 October 2019.
  5. ^abcMasiero, 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.
  6. ^abcdMainzer, 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.
  7. ^abcChang, 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.
  8. ^abcVeres, 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.
  9. ^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.
  10. ^"MPC/MPO/MPS Archive".Minor Planet Center. Retrieved30 April 2018.

External links

[edit]
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