1443 Ruppina

1443 Ruppina
Discovery [1]
Discovered by K. Reinmuth
Discovery site Heidelberg Obs.
Discovery date 29 December 1937
Designations
MPC designation (1443) Ruppina
Named after
 Ruppin (German city)[2]
1937 YG · 1931 TX3
main-belt · (outer) [3]
Orbital characteristics [1]
Epoch 4 September 2017 (JD 2458000.5)
Uncertainty parameter 0
Observation arc 85.20 yr (31,121 days)
Aphelion 3.1266 AU
Perihelion 2.7496 AU
2.9381 AU
Eccentricity 0.0642
5.04 yr (1,840 days)
61.181°
0° 11m 44.52s / day
Inclination 1.9299°
174.89°
163.11°
Physical characteristics
Dimensions 16.467±0.127 km[4]
16.67±0.75 km[5]
16.713±0.173 km[6]
18±3 km[7]
32.18 km (derived)[3]
5.880±0.001 h[8]
5.890±0.040 h[9]
5.9046±0.0347 h[10]
0.057 (assumed)[3]
0.176±0.017[5]
0.20±0.07[7]
0.2128±0.0392[6]
0.218±0.035[4]
C [3]
10.924±0.001 (R)[10] · 10.970±0.120 (R)[9] · 11.0[1] · 11.19±0.03[7] · 11.19[3][6] · 11.40[5]

    1443 Ruppina, provisional designation 1937 YG, is an asteroid from the outer region of the asteroid belt, approximately 17 kilometers in diameter. It was discovered on 29 December 1937, by German astronomer Karl Reinmuth at Heidelberg Observatory in southwest Germany.[11] It is named for the German city Ruppin.[2]

    Orbit and classification

    Ruppina asteroid orbits the Sun in the outer main-belt at a distance of 2.7–3.1 AU once every 5.04 years (1,840 days). Its orbit has an eccentricity of 0.06 and an inclination of 2° with respect to the ecliptic.[1] In 1931, Ruppina was first identified as 1931 TX3 at Lowell Observatory, extending the body's observation arc by 6 years prior to its official discovery at Heidelberg.[11]

    Physical characteristics

    Rotation period

    In November 2007, the first rotational lightcurve of Ruppina was obtained at Whitin Observatory in Massachusetts, United States. Lightcurve analysis gave a well-defined rotation period of 5.880 hours with a brightness variation of 0.35 magnitude (U=3).[7] During the 2014-apparition of Ruppina, an identical period was obtained again at Whitin Observatory (U=3),[8] while photometric observations in the R-band at the Palomar Transient Factory in California, gave a period of 5.890 and 5.9046 hours with an amplitude of 0.27 and 0.28, respectively (U=2/2).[9][10]

    Diameter and albedo

    According to the surveys carried out by the Japanese Akari satellite and NASA's Wide-field Infrared Survey Explorer with its subsequent NEOWISE mission, Ruppina measures approximately 16.5 kilometers in diameter and its surface has an albedo of 0.176 and 0.21, respectively.[4][5][6] Observations at the Whitin Observatory gave an albedo of 0.20 and a diameter of 18 kilometers,[7] while the Collaborative Asteroid Lightcurve Link assumes a standard albedo for carbonaceous C-type asteroids of 0.057, and consequently derives a much larger diameter of 32.18 kilometers with an absolute magnitude of 11.19.[3]

    Naming

    This minor planet is named for the German city of Ruppin, birthplace of astronomer Martin Ebell, who proposed the name and after whom the minor planet 1205 Ebella is named.[2] The official naming citation was published in The Names of the Minor Planets by Paul Herget in 1955 (H 130).[2]

    References

    1. 1 2 3 4 "JPL Small-Body Database Browser: 1443 Ruppina (1937 YG)" (2016-12-25 last obs.). Jet Propulsion Laboratory. Retrieved 25 July 2017.
    2. 1 2 3 4 Schmadel, Lutz D. (2007). Dictionary of Minor Planet Names – (1443) Ruppina. Springer Berlin Heidelberg. p. 116. ISBN 978-3-540-00238-3. Retrieved 5 January 2017.
    3. 1 2 3 4 5 6 "LCDB Data for (1443) Ruppina". Asteroid Lightcurve Database (LCDB). Retrieved 5 January 2017.
    4. 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. Bibcode:2014ApJ...791..121M. arXiv:1406.6645 Freely accessible. doi:10.1088/0004-637X/791/2/121. Retrieved 5 January 2017.
    5. 1 2 3 4 Usui, Fumihiko; Kuroda, Daisuke; Müller, Thomas G.; Hasegawa, Sunao; Ishiguro, Masateru; Ootsubo, Takafumi; et al. (October 2011). "Asteroid Catalog Using Akari: AKARI/IRC Mid-Infrared Asteroid Survey" (PDF). Publications of the Astronomical Society of Japan. 63 (5): 1117–1138. Bibcode:2011PASJ...63.1117U. doi:10.1093/pasj/63.5.1117. Retrieved 5 January 2017.
    6. 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" (PDF). The Astrophysical Journal. 741 (2): 25. Bibcode:2011ApJ...741...90M. arXiv:1109.6407 Freely accessible. doi:10.1088/0004-637X/741/2/90. Retrieved 5 January 2017.
    7. 1 2 3 4 5 Neugent, Kathryn F.; Slivan, Stephen M. (September 2008). "Rotation Periods and H Magnitudes of Two Koronis Family Members". The Minor Planet Bulletin. 35 (3): 116–118. Bibcode:2008MPBu...35..116N. ISSN 1052-8091. Retrieved 5 January 2017.
    8. 1 2 Arredondo, Anicia; Hartt, Anne-Marie; Yazdi, Sormeh K. (October 2014). "Rotation Periods and R Magnitudes of Three Koronis Family Members". The Minor Planet Bulletin. 41 (4): 252–254. Bibcode:2014MPBu...41..252A. ISSN 1052-8091. Retrieved 5 January 2017.
    9. 1 2 3 Chang, Chan-Kao; Ip, Wing-Huen; Lin, Hsing-Wen; Cheng, Yu-Chi; Ngeow, Chow-Choong; Yang, Ting-Chang; et al. (August 2015). "Asteroid Spin-rate Study Using the Intermediate Palomar Transient Factory". The Astrophysical Journal Supplement Series. 219 (2): 19. Bibcode:2015ApJS..219...27C. arXiv:1506.08493 Freely accessible. doi:10.1088/0067-0049/219/2/27. Retrieved 5 January 2017.
    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. Bibcode:2015AJ....150...75W. arXiv:1504.04041 Freely accessible. doi:10.1088/0004-6256/150/3/75. Retrieved 5 January 2017.
    11. 1 2 "1443 Ruppina (1937 YG)". Minor Planet Center. Retrieved 5 January 2017.
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