3714 Kenrussell

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3714 Kenrussell
Discovery  [1]
Discovered by E. Bowell
Discovery site Anderson Mesa Stn.
Discovery date12 October 1983
Designations
(3714) Kenrussell
Named after
 Kenneth S. Russell
(Australian astronomer) [2]
1983 TT1 ·1973 FK
1979 XT ·1981 FH1
1987 ST2
main-belt  ·(middle)
Eunomia   [3] [4]
Orbital characteristics   [1]
Epoch 23 March 2018 (JD 2458200.5)
Uncertainty parameter 0
Observation arc 44.82 yr (16,370 d)
Aphelion 3.0171 AU
Perihelion 2.1090 AU
2.5630 AU
Eccentricity 0.1771
4.10 yr (1,499 days)
121.37°
0° 14m 24.72s / day
Inclination 14.362°
29.616°
22.848°
Physical characteristics
Dimensions8.36 km (calculated) [3]
10.440±2.413 km [5]
11.260±0.108 km [6] [7]
5.2518±0.0005 h [8]
0.1057±0.0228 [6] [7]
0.1189±0.0615 [5]
0.21 (assumed) [3]
S (assumed) [3]
12.70 [1] [3] [5]  ·12.8 [7]

    3714 Kenrussell, provisional designation 1983 TT1, is a Eunomian asteroid from the central regions of the asteroid belt, approximately 10 kilometers (6 miles) in diameter. It was discovered on 12 October 1983, by American astronomer Edward Bowell at the Anderson Mesa Station near Flagstaff, Arizona, in the United States. It was named for Australian astronomer Kenneth S. Russell. [2] The presumably stony asteroid has a rotation period of 5.25 hours. [3]

    Contents

    Orbit and classification

    Kenrussell is a member of the Eunomia family ( 502 ), [3] [4] a prominent family of stony asteroids and the largest one in the intermediate main belt with more than 5,000 identified members. [9] : 23 

    It orbits the Sun in the central asteroid belt at a distance of 2.1–3.0  AU once every 4 years and 1 month (1,499 days; semi-major axis 2.56 AU). Its orbit has an eccentricity of 0.18 and an inclination of 14° with respect to the ecliptic. [1]

    The body's observation arc begins with its first observation as 1973 FK at the Cerro El Roble Station in March 1973, more than 10 years prior to its official discovery observation at Anderson Mesa. [2]

    Physical characteristics

    Based on its family membership, Kenrussell is an assumed stony S-type asteroid. [3]

    Rotation period

    In December 2016, a rotational lightcurve of Kenrussell was obtained from photometric observations by French amateur astronomer Matthieu Conjat . Lightcurve analysis gave a well-defined rotation period of 5.2518 hours with a brightness amplitude of 0.28 magnitude ( U=3 ). [8]

    Diameter and albedo

    According to the survey carried out by the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer, Kenrussell measures 10.440 and 11.260 kilometers in diameter and its surface has an albedo of 0.1189 and 0.1057, respectively. [5] [6] [7]

    The Collaborative Asteroid Lightcurve Link assumes an albedo of 0.21 – derived from 15 Eunomia, the family's parent body – and calculates a diameter of 8.36 kilometers based on an absolute magnitude of 12.7. [3]

    Naming

    This minor planet was named after Australian astronomer Kenneth S. Russell, a long-time operator of the 1.2-metre UK Schmidt Telescope at the Siding Spring Observatory in Australia. He is a discoverer of minor planets, (17483) and (306376) as well as several periodic comets including 83D/Russell, 89P/Russell, 91P/Russell and 94P/Russell. The official naming citation was published by the Minor Planet Center on 31 May 1988 (M.P.C. 13177). [10]

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    References

    1. 1 2 3 4 "JPL Small-Body Database Browser: 3714 Kenrussell (1983 TT1)" (2018-01-22 last obs.). Jet Propulsion Laboratory . Retrieved 13 February 2018.
    2. 1 2 3 "3714 Kenrussell (1983 TT1)". Minor Planet Center. Retrieved 13 February 2018.
    3. 1 2 3 4 5 6 7 8 9 "LCDB Data for (3714) Kenrussell". Asteroid Lightcurve Database (LCDB). Retrieved 13 February 2018.
    4. 1 2 "Asteroid 3714 Kenrussell – Nesvorny HCM Asteroid Families V3.0". Small Bodies Data Ferret. Retrieved 26 October 2019.
    5. 1 2 3 4 Masiero, Joseph R.; Nugent, C.; Mainzer, A. K.; Wright, E. L.; Bauer, J. M.; Cutri, R. M.; et al. (October 2017). "NEOWISE Reactivation Mission Year Three: Asteroid Diameters and Albedos". The Astronomical Journal. 154 (4): 10. arXiv: 1708.09504 . Bibcode:2017AJ....154..168M. doi: 10.3847/1538-3881/aa89ec .
    6. 1 2 3 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.
    7. 1 2 3 4 Mainzer, 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.
    8. 1 2 Behrend, Raoul. "Asteroids and comets rotation curves – (3714) Kenrussell". Geneva Observatory . Retrieved 13 February 2018.
    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. Retrieved 13 February 2018.
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