16879 Campai

16879 Campai, provisional designation 1998 BH10, is a stony Witt asteroid and slow rotator from the central region of the asteroid belt, approximately 10 kilometers (6 miles) in diameter. The S-type asteroid was discovered on 24 January 1998, by Italian astronomers Andrea Boattini and Maura Tombelli at the Pistoia Mountains Astronomical Observatory in San Marcello Pistoiese, Tuscany, central Italy.[1] It was named for Italian amateur astronomer Paolo Campai.[2]

16879 Campai
Discovery [1]
Discovered byA. Boattini
M. Tombelli
Discovery sitePistoia Mountains Obs.
Discovery date24 January 1998
Designations
(16879) Campai
Named after
Paolo Campai [2]
(Italian amateur astronomer)
1998 BH10
main-belt [1][3] · (middle)
Witt [4]
Orbital characteristics [3]
Epoch 23 March 2018 (JD 2458200.5)
Uncertainty parameter 0
Observation arc39.78 yr (14,529 d)
Aphelion2.8229 AU
Perihelion2.6938 AU
2.7584 AU
Eccentricity0.0234
4.58 yr (1,673 d)
349.41°
0° 12m 54.36s / day
Inclination7.1221°
47.289°
230.77°
Physical characteristics
Mean diameter
10.61 km (calculated)[5]
314.2468±4.9149 h[6]
0.057 (assumed)[5]
S [7] · C (assumed)[5]
12.97±0.46[7]
13.150±0.005[6]
13.3[3] · 13.6[5]

    Orbit and classification

    Campai is a member of the Witt family (535),[4] a large family of (predominantly) stony asteroids with more than 1,600 known members.[8] It orbits the Sun in the central main-belt at a distance of 2.7–2.8 AU once every 4 years and 7 months (1,673 days; semi-major axis of 2.76 AU). Its orbit has an eccentricity of 0.02 and an inclination of 7° with respect to the ecliptic.[3] The first precovery was obtained at Siding Spring Observatory in July 1977, extending the asteroid's observation arc by 22 years prior to its discovery.[1]

    Physical characteristics

    Campai has been characterized as a common, stony S-type asteroid,[5] in line with the overall spectral type for members of the Witt family.[8]:23

    Slow rotator

    In October 2010, a rotational lightcurve of Campai was obtained from photometric observations made at the Palomar Transient Factory in California. It rendered an exceptionally long period of 314.2468±4.9149 hours with a brightness amplitude of 0.68 magnitude (U=2).[6] While the result is based on less than full coverage, and may be refined by future observations, Campai is one of the slowest rotating asteroids known to exist.

    Diameter and albedo

    The Collaborative Asteroid Lightcurve Link calculates a diameter of 10.5 kilometers with an absolute magnitude of 13.6 and an assumed standard albedo for a carbonaceous asteroid of 0.057.[5]

    Naming

    This minor planet was named for Italian amateur astronomer Paolo Campai (born 1957) from Florence, who is specialized in teaching and astrophotography. Both discoverers made his acquaintance near Florence on a night in 1985, while observing comet 1P/Halley and α Phoenicis.[2] The approved naming citation was published by the Minor Planet Center on 6 August 2003 (M.P.C. 49281).[9]

    gollark: The pattern matching is very coil.
    gollark: Or it would if I didn't just inefficiently clone the trees near-continuously.
    gollark: osmarkscalculator™ suffers from this somewhat.
    gollark: Anyway, I've found that Rust makes some scenarios substantially more annoying. Mostly when dealing with weird trees and such a GC would handle nicely.
    gollark: How bad.

    References
    1. "16879 Campai (1998 BH10)". Minor Planet Center. Retrieved 22 March 2016.
    2. Schmadel, Lutz D. (2006). "(16879) Campai [2.76, 0.02, 7.1]". Dictionary of Minor Planet Names – (16879) Campai, Addendum to Fifth Edition: 2003–2005. Springer Berlin Heidelberg. p. 102. doi:10.1007/978-3-540-34361-5_1067. ISBN 978-3-540-34360-8.
    3. "JPL Small-Body Database Browser: 16879 Campai (1998 BH10)" (2017-05-01 last obs.). Jet Propulsion Laboratory. Retrieved 26 June 2017.
    4. "Asteroid 16879 Campai – Nesvorny HCM Asteroid Families V3.0". Small Bodies Data Ferret. Retrieved 27 October 2019.
    5. "LCDB Data for (16879) Campai". Asteroid Lightcurve Database (LCDB). Retrieved 17 May 2016.
    6. 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. 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.
    8. 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.
    9. "MPC/MPO/MPS Archive". Minor Planet Center. Retrieved 17 May 2016.

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