133528 Ceragioli

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133528 Ceragioli
Discovery [1]
Discovered by D. Healy
Discovery site Junk Bond Obs.
Discovery date4 October 2003
Designations
(133528) Ceragioli
Named after
 Roger Ceragioli [1]
(American optician)
2003 TC2
main-belt [1] [2]  ·( outer )
Koronis [3] [4]
Orbital characteristics [2]
Epoch 27 April 2019 (JD 2458600.5)
Uncertainty parameter 0
Observation arc 17.73 yr (6,476 d)
Aphelion 3.1087 AU
Perihelion 2.6053 AU
2.8570 AU
Eccentricity 0.0881
4.83 yr (1,764 d)
92.922°
0° 12m 14.76s / day
Inclination 1.2673°
334.80°
21.722°
Physical characteristics
1.75  km (calculated) [5]
3.052±0.0159  h [6]
0.24(assumed) [5]
S (assumed) [5]
15.498±0.008(R) [6]
15.5 [1] [2]

    133528 Ceragioli, provisional designation 2003 TC2, is an asteroid of the Koronis family from the outer regions of the asteroid belt, approximately 1.75 kilometers (1.1 miles) in diameter. It was discovered on 4 October 2003 by American astronomer David Healy at the Junk Bond Observatory in Arizona, United States. The likely stony and possibly elongated asteroid has a rotation period of 3.1 hours. [5] It was named for American optician Roger Ceragioli. [1]

    Contents

    Orbit and classification

    Ceragioli is a member of the Koronis family ( 605 ), [3] [4] a very large asteroid family with nearly co-planar ecliptical orbits and named after 158 Koronis. [7] It orbits the Sun in the outer asteroid belt at a distance of 2.6–3.1  AU once every 4 years and 10 months (1,764 days; semi-major axis of 2.86 AU). Its orbit has an eccentricity of 0.09 and an inclination of 1° with respect to the ecliptic. [2] The body's observation arc begins with a precovery taken by Spacewatch in September 1998, or 5 years prior to its official discovery observation at the Junk Bond Observatory. [1]

    Naming

    This minor planet was named after American optician Roger Ceragioli (born 1959) at the Steward Observatory Mirror Laboratory, whose projects include parts of the Bok Telescope and the MODS spectrograph for the Large Binocular Telescope. The official naming citation was published by the Minor Planet Center on 1 June 2007 ( M.P.C. 59925). [8]

    Physical characteristics

    Ceragioli is an assumed stony S-type asteroid, [5] in line with the overall spectral type for members of the Koronis family. [7]

    Rotation period

    In February 2010, a rotational lightcurve of Ceragioli was obtained from photometric observations in the R-band by astronomers at the Palomar Transient Factory in California. Lightcurve analysis gave a rotation period of 3.052±0.0159 hours with a brightness variation of 0.35 magnitude ( U=2 ), indicative of an elongated shape. [6] Also in February 2010, David Polishook determined a similar period of 3.06±0.04 hours with an amplitude of 0.25 magnitude ( U=1+ ). [9]

    Diameter and albedo

    The Collaborative Asteroid Lightcurve Link assumes an albedo of 0.24 and calculates a diameter of 1.75 kilometers based on an absolute magnitude of 15.95. [5]

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    References

    1. 1 2 3 4 5 6 "133528 Ceragioli (2003 TC2)". Minor Planet Center. Retrieved 3 December 2018.
    2. 1 2 3 4 "JPL Small-Body Database Browser: 133528 Ceragioli (2003 TC2)" (2016-06-06 last obs.). Jet Propulsion Laboratory . Retrieved 3 December 2018.
    3. 1 2 "Asteroid 133528 Ceragioli". Small Bodies Data Ferret. Retrieved 3 December 2018.
    4. 1 2 "Asteroid (133528) Ceragioli". AstDyS-2, Asteroids – Dynamic Site. Retrieved 3 December 2018.
    5. 1 2 3 4 5 6 "LCDB Data for (133528) Ceragioli". Asteroid Lightcurve Database (LCDB). Retrieved 3 December 2018.
    6. 1 2 3 Waszczak, Adam; Chang, Chan-Kao; Ofek, Eran O.; Laher, Russ; Masci, Frank; Levitan, David; et al. (September 2015). "Asteroid Light Curves from the Palomar Transient Factory Survey: Rotation Periods and Phase Functions from Sparse Photometry". The Astronomical Journal. 150 (3): 35. arXiv: 1504.04041 . Bibcode:2015AJ....150...75W. doi:10.1088/0004-6256/150/3/75.
    7. 1 2 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.
    8. ↑ "MPC/MPO/MPS Archive". Minor Planet Center. Retrieved 3 December 2018.
    9. ↑ Polishook, D.; Ofek, E. O.; Waszczak, A.; Kulkarni, S. R.; Gal-Yam, A.; Aharonson, O.; et al. (April 2012). "Asteroid rotation periods from the Palomar Transient Factory survey". Monthly Notices of the Royal Astronomical Society. 421 (3): 2094–2108. arXiv: 1201.1930 . Bibcode:2012MNRAS.421.2094P. doi: 10.1111/j.1365-2966.2012.20462.x .
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