10830 Desforges
Discovery[1]
Discovered byE. W. Elst
Discovery siteLa Silla Obs.
Discovery date20 October 1993
Designations
(10830) Desforges
Named after
Jacques Desforges[1]
(French priest)
1993 UT6 · 1982 FS2
1984 SS7
main-belt[1][2] · (middle)
background[3] · Eunomia[4]
Orbital characteristics[2]
Epoch 23 March 2018 (JD 2458200.5)
Uncertainty parameter 0
Observation arc35.27 yr (12,884 d)
Aphelion3.1271 AU
Perihelion2.1944 AU
2.6607 AU
Eccentricity0.1753
4.34 yr (1,585 d)
151.24°
0° 13m 37.56s / day
Inclination11.153°
178.72°
307.82°
Physical characteristics
Mean diameter
4.21 km (calculated)[4]
7.692±2.245 km[5]
9.390±0.203 km[6][7]
8.804±0.0058 h[8]
0.0635±0.0545[5]
0.0797±0.0101[7]
0.080±0.010[6]
0.21 (assumed)[4]
S (assumed)[4]
13.5[7]
13.6[2]
13.739±0.008 (R)[8]
14.18[5][9]
14.19[4]

    10830 Desforges, provisional designation 1993 UT6, is a background or Eunomian asteroid from the central regions of the asteroid belt, approximately 7 kilometers (4 miles) in diameter. It was discovered on 20 October 1993, by Belgian astronomer Eric Elst at the La Silla Observatory in northern Chile.[1] The likely elongated S-type asteroid has a rotation period of 8.8 hours.[4] It was named after French priest and aviation visionary Jacques Desforges.[1]

    Orbit and classification

    Desforges is a non-family asteroid of the main belt's background population when applying the hierarchical clustering method to its proper orbital elements.[3] Based on osculating Keplerian orbital elements, the asteroid has also been classified as a member of the Eunomia family (502), a prominent family of stony S-type asteroid and the largest one in the intermediate main belt with more than 5,000 members.[4]

    It orbits the Sun in the central main-belt at a distance of 2.2–3.1 AU once every 4 years and 4 months (1,585 days; semi-major axis of 2.66 AU). Its orbit has an eccentricity of 0.18 and an inclination of 11° with respect to the ecliptic.[2] The body's observation arc begins with its first observations as 1982 FS2 at Klet Observatory in March 1982, more than 11 years prior to its official discovery observation at La Silla.[1]

    Physical characteristics

    Desforges is an assumed stony S-type asteroid,[4] which is the overall spectral type for members of the Eunomia family.[10]: 23  Observations with the Wide-field Infrared Survey Explorer (WISE), however, gave a low geometric albedo more typical for an X- or C-type asteroid (see below).

    Rotation period

    In August 2010, a rotational lightcurve of Desforges was obtained from photometric observations in the R-band by astronomers at the Palomar Transient Factory in California.[8] Lightcurve analysis gave a rotation period of 8.804 hours with a high brightness amplitude of 0.69 magnitude, which indicates that the body has a non-spherical shape (U=2).[4]

    Diameter and albedo

    According to the survey carried out by the NEOWISE mission of NASA's WISE telescope, Desforges measures between 7.692 and 9.390 kilometers in diameter and its surface has an albedo between 0.0635 and 0.080.[5][6][7]

    The Collaborative Asteroid Lightcurve Link assumes an albedo of 0.21 – derived from the Eunomia family's parent body, 15 Eunomia – and calculates a diameter of 4.21 kilometers based on an absolute magnitude of 14.19.[4]

    Naming

    This minor planet was named after a French priest Jacques Desforges (1723–1791), who was imprisoned for eight months in 1758 in the Bastille, during which time he planned the construction of a flying machine.[1] The official naming citation was published by the Minor Planet Center on 18 March 2003 (M.P.C. 48156).[11]

    References

    1. 1 2 3 4 5 6 7 "10830 Desforges (1993 UT6)". Minor Planet Center. Retrieved 1 May 2018.
    2. 1 2 3 4 "JPL Small-Body Database Browser: 10830 Desforges (1993 UT6)" (2017-07-05 last obs.). Jet Propulsion Laboratory. Retrieved 1 May 2018.
    3. 1 2 "Asteroid 10830 Desforges – Proper Elements". AstDyS-2, Asteroids – Dynamic Site. Retrieved 29 October 2019.
    4. 1 2 3 4 5 6 7 8 9 10 "LCDB Data for (10830) Desforges". Asteroid Lightcurve Database (LCDB). Retrieved 1 May 2018.
    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 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.
    9. ↑ 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.
    10. ↑ 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.
    11. ↑ "MPC/MPO/MPS Archive". Minor Planet Center. Retrieved 1 May 2018.
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