6882 Sormano

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6882 Sormano
006882-asteroid shape model (6882) Sormano.png
Shape model of Sormano from its lightcurve
Discovery [1]
Discovered by P. Sicoli
V. Giuliani
Discovery site Sormano Obs.
Discovery date5 February 1995
Designations
(6882) Sormano
Named after
 Sormano Observatory
(discovering observatory) [2]
1995 CC1 ·1986 XM2
1989 OW ·1993 OQ
Orbital characteristics [3]
Epoch 4 September 2017 (JD 2458000.5)
Uncertainty parameter 0
Observation arc 27.85 yr (10,173 days)
Aphelion 2.8043 AU
Perihelion 2.2997 AU
2.5520 AU
Eccentricity 0.0989
4.08 yr (1,489 days)
327.31°
0° 14m 30.48s / day
Inclination 14.390°
284.19°
16.030°
Physical characteristics
6.69 km (calculated) [4]
7.665±0.101 km [5]
8.096±0.040 km [6]
3.6901±0.0006  h [7]
3.998344±0.000001 h [8]
0.21 (assumed) [4]
0.269±0.034 [6]
0.3003±0.0545 [5]
S (family-based) [4]
12.5 [5]  ·12.7 [3]  ·12.736±0.003(R) [7]  ·13.19 [4]

    6882 Sormano (prov. designation: 1995 CC1) is an stony Eunomia asteroid from the middle region of the asteroid belt, approximately 7 kilometers (4.3 miles) in diameter. It was discovered on 5 February 1995, by Italian amateur astronomers Piero Sicoli and Valter Giuliani at Sormano Astronomical Observatory in northern Italy. [1] The asteroid was named for the Italian mountain-village of Sormano and its discovering observatory. [2]

    Contents

    Orbit and classification

    Sormano is a member of the Eunomia family, a large group of S-type asteroids and the most prominent family in the intermediate main-belt. It orbits the Sun at a distance of 2.3–2.8  AU once every 4 years and 1 month (1,489 days). Its orbit has an eccentricity of 0.10 and an inclination of 14° with respect to the ecliptic. [3] The asteroid's observation arc begins 6 years prior to its discovery, as it had previously been observed as 1989 OW at Palomar Observatory in 1989. [1]

    Naming

    This minor planet was named in honor of the Italian mountain-village of Sormano and its discovering nearby observatory. It is funded, built and operated by the "Gruppo Astrofili Brianza", a group of Italian amateur astronomers who have discovered numerous minor planets. [2] The official naming citation was published by the Minor Planet Center on 3 May 1996 ( M.P.C. 27130). [9]

    Physical characteristics

    Rotation and shape

    In September 2010, a rotational lightcurve of Sormano was obtained from photometric observations made at the Palomar Transient Factory in California. It gave a rotation period of 3.6901 hours with a high brightness variation of 0.71 magnitude, indicative of a non-spheroidal shape ( U=2 ). [7] A similar period of 3.998 hours was derived from remodeled data of the Lowell photometric database ( n.a. ). [8]

    Diameter and albedo

    According to the survey carried out by NASA's Wide-field Infrared Survey Explorer with its subsequent NEOWISE mission, Sormano measures 7.6 to 8.0 kilometers in diameter and its surface has an albedo between 0.269 and 0.300. [5] [6] The Collaborative Asteroid Lightcurve Link assumes an albedo 0.21 – derived from 15 Eunomia, the family's largest member and namesake – and calculates a diameter of 6.69 kilometers with an absolute magnitude of 13.19. [4]

    References

    1. 1 2 3 4 "6882 Sormano (1995 CC1)". Minor Planet Center. Retrieved 4 November 2016.
    2. 1 2 3 Schmadel, Lutz D. (2007). "(6882) Sormano". Dictionary of Minor Planet Names . Springer Berlin Heidelberg. p.  563. doi:10.1007/978-3-540-29925-7_6162. ISBN   978-3-540-00238-3.
    3. 1 2 3 4 "JPL Small-Body Database Browser: 6882 Sormano (1995 CC1)" (2017-06-05 last obs.). Jet Propulsion Laboratory . Retrieved 21 June 2017.
    4. 1 2 3 4 5 6 7 "LCDB Data for (6882) Sormano". Asteroid Lightcurve Database (LCDB). Retrieved 4 November 2016.
    5. 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. S2CID   118700974.
    6. 1 2 3 Masiero, Joseph R.; Grav, T.; Mainzer, A. K.; Nugent, C. R.; Bauer, J. M.; Stevenson, R.; et al. (August 2014). "Main-belt Asteroids with WISE/NEOWISE: Near-infrared Albedos". The Astrophysical Journal. 791 (2): 11. arXiv: 1406.6645 . Bibcode:2014ApJ...791..121M. doi:10.1088/0004-637X/791/2/121. S2CID   119293330 . Retrieved 4 November 2016.
    7. 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. S2CID   8342929 . Retrieved 4 November 2016.
    8. 1 2 Durech, J.; Hanus, J.; Oszkiewicz, D.; Vanco, R. (March 2016). "Asteroid models from the Lowell photometric database". Astronomy and Astrophysics. 587: 6. arXiv: 1601.02909 . Bibcode:2016A&A...587A..48D. doi:10.1051/0004-6361/201527573. S2CID   118427201 . Retrieved 4 November 2016.
    9. ↑ "MPC/MPO/MPS Archive". Minor Planet Center. Retrieved 4 November 2016.
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