(16882) 1998 BO13

(16882) 1998 BO13, provisional designation 1998 BO13, is a dark Zhongguo asteroid from the background population in the outermost region of the asteroid belt, approximately 10 kilometers (6 miles) in diameter. It was discovered on 24 January 1998, by astronomers with the Lincoln Near-Earth Asteroid Research at the Lincoln Laboratory's Experimental Test Site near Socorro, New Mexico, in the United States.[1]

(16882) 1998 BO13
Discovery [1]
Discovered byLINEAR
Discovery siteLincoln Lab's ETS
Discovery date24 January 1998
Designations
(16882) 1998 BO13
1998 BO13 · 1999 JC21
main-belt [1] · (outer) [2]
Zhongguo [3] · 2:1 res [4]
Orbital characteristics [2]
Epoch 23 March 2018 (JD 2458200.5)
Uncertainty parameter 0
Observation arc20.49 yr (7,483 d)
Aphelion3.9425 AU
Perihelion2.6761 AU
3.3093 AU
Eccentricity0.1913
6.02 yr (2,199 d)
57.356°
0° 9m 49.32s / day
Inclination0.5370°
339.83°
225.85°
Physical characteristics
Mean diameter
9.827±0.226 km[5]
0.061±0.010[5]
13.5[2]

    Orbit and classification

    1998 BO13 is a non-family asteroid from the main belt's background population,[6] and a member of the small group of Zhongguo asteroids,[3] located in the Hecuba gap and locked in a 2:1 mean-motion resonance with the gas giant Jupiter. Contrary to the nearby Griqua group, the orbits of the Zhongguos are stable over half a billion years.[3] According to Milani and Knežević, this asteroid is a core member of the unnamed asteroid family formed by the Zhongguo asteroid (11097) 1994 UD1.[4]

    It orbits the Sun in the outer main-belt at a distance of 2.7–3.9 AU once every 6.02 years (2,199 days; semi-major axis of 3.31 AU). Its orbit has an eccentricity of 0.19 and an inclination of 1° with respect to the ecliptic.[2]

    The body's observation arc begins with a precovery taken by Spacewatch in November 1996, or 14 months prior to its official discovery observation at Socorro.[1]

    Physical characteristics

    1998 BO13 has an absolute magnitude of 13.5.[2] As of 2018, no rotational lightcurve for this asteroid has been obtained from photometric observations. The body's rotation period, pole and shape remain unknown.[2]

    Diameter and albedo

    According to the survey carried out by the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer, measures 9.827 kilometers in diameter and its surface has an albedo of 0.061,[5] which is rather typical for the abundant carbonaceous C-type asteroids in the outer main-belt.

    Numbering and naming

    This minor planet was numbered by the Minor Planet Center on 13 September 2000, after its orbit had sufficiently been secured (M.P.C. 41165).[7] As of 2018, it has not been named.[1]

    References
    1. "16882 (1998 BO13)". Minor Planet Center. Retrieved 26 April 2018.
    2. "JPL Small-Body Database Browser: 16882 (1998 BO13)" (2017-05-03 last obs.). Jet Propulsion Laboratory. Retrieved 26 April 2018.
    3. Roig, F.; Nesvorný, D.; Ferraz-Mello, S. (September 2002). "Asteroids in the 2 : 1 resonance with Jupiter: dynamics and size distribution [ Erratum: 2002MNRAS.336.1391R ]". Monthly Notices of the Royal Astronomical Society. 335 (2): 417–431. Bibcode:2002MNRAS.335..417R. doi:10.1046/j.1365-8711.2002.05635.x. Retrieved 26 April 2018.
    4. "Asteroid (16882) 1998 BO13 – Proper Elements". AstDyS-2, Asteroids – Dynamic Site. Retrieved 29 October 2019.
    5. 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 26 April 2018.
    6. "Small Bodies Data Ferret". Nesvorny HCM Asteroid Families V3.0. Archived from the original on 2 August 2017. Retrieved 26 April 2018.
    7. "MPC/MPO/MPS Archive". Minor Planet Center. Retrieved 26 April 2018.

    This article is issued from Wikipedia. The text is licensed under Creative Commons - Attribution - Sharealike. Additional terms may apply for the media files.