1145 Robelmonte

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1145 Robelmonte
Discovery [1]
Discovered by E. Delporte
Discovery site Uccle Obs.
Discovery date3 February 1929
Designations
(1145) Robelmonte
Named after
 Robelmont [2]
(birthplace of Sylvain Arend)
1929 CC ·A915 RN
main-belt  · Vestian [3] [4]
Orbital characteristics [1]
Epoch 4 September 2017 (JD 2458000.5)
Uncertainty parameter 0
Observation arc 86.87 yr (31,730 days)
Aphelion 2.7112 AU
Perihelion 2.1363 AU
2.4238 AU
Eccentricity 0.1186
3.77 yr (1,378 days)
68.012°
0° 15m 40.32s / day
Inclination 6.2071°
346.82°
267.51°
Physical characteristics
Dimensions18.85±5.08 km [5]
19.13±5.00 km [6]
22.23±0.39 km [7]
23.16 km (derived) [3]
24.029±0.129 km [7]
24.07±0.37 km [8]
24.757±0.541 km [9]
7.582±0.0027 h [10]
8.002±0.002 h [11]
9.01±0.01 h [12]
21 h [13]
0.0994 (derived) [3]
0.1046±0.0175 [9]
0.108±0.020 [7]
0.113±0.004 [8]
0.128±0.006 [14]
0.15±0.09 [6]
0.16±0.08 [5]
S [3]
11.10 [8] [9]  ·11.157±0.001(R) [10]  ·11.30 [3] [5] [7]  ·11.37±0.27 [15]  ·11.4 [1]  ·11.44 [6]

    1145 Robelmonte, provisional designation 1929 CC, is a Vestian asteroid from the inner regions of the asteroid belt, approximately 23 kilometers in diameter.

    Contents

    It was discovered on 3 February 1929, by Belgian astronomer Eugène Delporte at the Royal Observatory of Belgium in Uccle. [16] Through a glitch in the naming process, the asteroid received the name "Robelmonte" instead of "Mimi" as originally intended by the discoverer. [2]

    Orbit and classification

    Robelmonte is a member of the Vesta family ( 401 ), [3] [4] the main-belt's second-largest asteroid family by number of members. [17] : 23  Vestian asteroids have a composition akin to the HED meteorites and are thought to have originated deep within 4 Vesta's crust, possibly from Rheasilvia, a large impact crater on its southern hemisphere near the South pole, formed as a result of a subcatastrophic collision. [18] Vesta is the main belt's second-largest and second-most-massive body after Ceres.

    Robelmonte orbits the Sun in the inner main-belt at a distance of 2.1–2.7  AU once every 3 years and 9 months (1,378 days). Its orbit has an eccentricity of 0.12 and an inclination of 6° with respect to the ecliptic. [1] The asteroid was first identified as A915 RN at Simeiz Observatory in September 1915. Its observation arc begins at Algiers Observatory in August 1930, more than a year after its official discovery observation at Uccle. [16]

    Physical characteristics

    Robelmonte is an assumed stony S-type asteroid, [3] despite its relatively low albedo.

    Rotation period

    In March 2016, the best-rated rotational lightcurve of Robelmonte was obtained from photometric observations by the Spanish amateur astronomer group OBAS (Observadores de Asteroides – Asteroid Observers). Lightcurve analysis gave a rotation period of 8.002 hours with a brightness variation of 0.13 magnitude ( U=3- ). [11] Previous observations gave a divergent period of 7.582, 9.01 and 21 hours, respectively ( U=2/2/1 ). [10] [12] [13]

    Diameter and albedo

    According to the surveys carried out by the Japanese Akari satellite and the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer, Robelmonte measures between 18.85 and 24.757 kilometers in diameter and its surface has an albedo between 0.1046 and 0.16. [5] [6] [7] [8] [9] [14]

    The Collaborative Asteroid Lightcurve Link derives a low albedo of 0.0994 and a diameter of 23.16 kilometers based on an absolute magnitude of 11.3. [3]

    Naming

    This minor planet was named after Robelmont, the birthplace of Belgian astronomer Sylvain Arend (Robelmonte is the feminine form). Through an error, the names intended for 1127 Mimi (wife of Delporte) and 1145 Robelmonte (birthplace of Arend) had been switched, and each name had been proposed by the discoverer of the other asteroid. The official naming citation was mentioned in The Names of the Minor Planets by Paul Herget in 1955 ( H 107 ). [2]

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    References

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    2. 1 2 3 Schmadel, Lutz D. (2007). "(1145) Robelmonte". Dictionary of Minor Planet Names. Springer Berlin Heidelberg. p. 97. doi:10.1007/978-3-540-29925-7_1146. ISBN   978-3-540-00238-3.
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    5. 1 2 3 4 Nugent, C. R.; Mainzer, A.; Masiero, J.; Bauer, J.; Cutri, R. M.; Grav, T.; et al. (December 2015). "NEOWISE Reactivation Mission Year One: Preliminary Asteroid Diameters and Albedos". The Astrophysical Journal. 814 (2): 13. arXiv: 1509.02522 . Bibcode:2015ApJ...814..117N. doi:10.1088/0004-637X/814/2/117 . Retrieved 8 September 2017.
    6. 1 2 3 4 Nugent, C. R.; Mainzer, A.; Bauer, J.; Cutri, R. M.; Kramer, E. A.; Grav, T.; et al. (September 2016). "NEOWISE Reactivation Mission Year Two: Asteroid Diameters and Albedos". The Astronomical Journal. 152 (3): 12. arXiv: 1606.08923 . Bibcode:2016AJ....152...63N. doi: 10.3847/0004-6256/152/3/63 .
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    10. 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 . Retrieved 8 September 2017.
    11. 1 2 Mansego, Enrique Arce; Rodriguez, Pedro Brines; de Haro, Juan Lozano; Chiner, Onofre Rodrigo; Silva, Alvaro Fornas; Porta, David Herrero; et al. (October 2016). "Eighteen Asteroids Lightcurves at Asteroides Observers (OBAS) - MPPD: 2016 March-May". The Minor Planet Bulletin. 43 (4): 332–336. Bibcode:2016MPBu...43..332M. ISSN   1052-8091 . Retrieved 8 September 2017.
    12. 1 2 Gartrelle, Gordon M. (April 2012). "Lightcurve Results for Eleven Asteroids". The Minor Planet Bulletin. 39 (2): 40%–46. Bibcode:2012MPBu...39...40G. ISSN   1052-8091 . Retrieved 8 September 2017.
    13. 1 2 Behrend, Raoul. "Asteroids and comets rotation curves – (1145) Robelmonte". Geneva Observatory . Retrieved 8 September 2017.
    14. 1 2 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 . Retrieved 8 September 2017.
    15. ↑ 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 . Retrieved 8 September 2017.
    16. 1 2 "1145 Robelmonte (1929 CC)". Minor Planet Center. Retrieved 8 September 2017.
    17. ↑ 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.
    18. ↑ Kelley, Michael S.; Vilas, Faith; Gaffey, Michael J.; Abell, Paul A. (September 2003). "Quantified mineralogical evidence for a common origin of 1929 Kollaa with 4 Vesta and the HED meteorites". Icarus. 165 (1): 215–218. Bibcode:2003Icar..165..215K. doi:10.1016/S0019-1035(03)00149-0 . Retrieved 8 September 2017.
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