1111 Reinmuthia

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1111 Reinmuthia
001111-asteroid shape model (1111) Reinmuthia.png
Shape model of Reinmuthia from its lightcurve
Discovery [1]
Discovered by K. Reinmuth
Discovery site Heidelberg Obs.
Discovery date11 February 1927
Designations
(1111) Reinmuthia
Named after
 Karl Reinmuth [2]
(the discoverer)
1927 CO ·1929 QG
Orbital characteristics [1]
Epoch 4 September 2017 (JD 2458000.5)
Uncertainty parameter 0
Observation arc 90.72 yr (33,137 days)
Aphelion 3.2947 AU
Perihelion 2.6911 AU
2.9929 AU
Eccentricity 0.1008
5.18 yr (1,891 days)
329.12°
0° 11m 25.44s / day
Inclination 3.8917°
132.44°
236.17°
Physical characteristics
Mean diameter
24.38±0.48 km [6]
41.26 km (derived) [7]
4.00742±0.00005  h [8]
4.007347 h [9]
4.00750±0.00003 h [8]
4.0075±0.0001 h [10] [lower-alpha 1]
4.02 h [11]
  • (356.0°, 68.0°) (λ1/β1) [5]
  • (153.0°, 78.0°) (λ2/β2) [5]
0.057 (assumed) [7]
0.167±0.008 [6]
Tholen = F XU: [1] [7]
B–V = 0.639±0.016 [1]
U–B = 0.230±0.030 [1]
10.65 [7] [11]  ·10.67 [1] [6]

    1111 Reinmuthia (prov. designation: 1927 CO) is a very elongated asteroid from the background population, located in the outer region of the asteroid belt. It was discovered on 11 February 1927, by German astronomer Karl Reinmuth at the Heidelberg Observatory in southwest Germany. [3] The F-type asteroid (FX) has a short rotation period of 4.02 hours and measures approximately 40 kilometers (25 miles) in diameter. [7] It was later named in honor of Karl Reinmuth, the discoverer himself. [2]

    Contents

    Orbit and classification

    Reinmuthia is a non-family asteroid of the main belt's background population when applying the hierarchical clustering method to its proper orbital elements. [4] [5] It orbits the Sun in the outer asteroid belt at a distance of 2.7–3.3  AU once every 5 years and 2 months (1,891 days; semi-major axis of 2.99 AU). Its orbit has an eccentricity of 0.10 and an inclination of 4° with respect to the ecliptic. [1] The body's observation arc begins at Heidelberg with its official discovery observation. [3]

    Naming

    This minor planet was named after its discoverer, Karl Reinmuth (1892–1979), a German astronomer at the Heidelberg-Königstuhl State Observatory and a prolific discoverer of minor planets. In total, he discovered 395 asteroids, most of them during the 1920s and 1930s, which was a unique record for many years. His discoveries include 1862 Apollo and 69230 Hermes, two lost asteroids and near-Earth objects as well as several large Jupiter trojans. His 1931-discovered asteroid (11435) 1931 UB is the oldest discovered yet still unnamed asteroid. The official naming citation was mentioned in The Names of the Minor Planets by Paul Herget in 1955 ( H 104 ). [2]

    Physical characteristics

    Lightcurve-based 3D inversion model of Reinmuthia 1111Reinmuthia (Lightcurve Inversion).png
    Lightcurve-based 3D inversion model of Reinmuthia

    In the Tholen classification, Reinmuthia has an ambiguous spectral type, closest to that of a dark F-type and somewhat similar to an X-type asteroid. The spectrum had also been flagged as "unusual" and "nosy" by Tholen (FXU:). [1]

    Rotation period

    Rotational lightcurves of Reinmuthia have been obtained from photometric observations by American astronomer Richard Binzel as well as by Hiromi and Hiroko Hamanowa at the Hamanowa Astronomical Observatory ( D91 ) in Japan ( U=3/3/3 ). [8] [10] [11] Lightcurve analysis gave a consolidated, well-defined rotation period of 4.02 hours with a high brightness amplitude between 0.61 and 0.95 magnitude ( U=3 ). [7] [lower-alpha 1]

    Poles and shape

    Lightcurve inversion also modeled the body's shape and poles. In 2013, modelling by an international study using photometric data from the US Naval Observatory, the Uppsala Asteroid Photometric Catalogue, the Palomar Transient Factory and the Catalina Sky Survey gave a similar sidereal period of 4.007347 hours and two spin axes of (356.0°, 68.0°) and (153.0°, 78.0°) in ecliptic coordinates (λ, β). The body's very elongated shape had already been indicated by the high brightness variation measured during the photometric observations. [9]

    Diameter and albedo

    According to the survey carried out by the Japanese Akari satellite, Reinmuthia measures 24.38 kilometers in diameter and its surface has an albedo of 0.167. [6] The Collaborative Asteroid Lightcurve Link assumes a standard albedo for carbonaceous asteroids of 0.057 and derives a diameter of 41.26 kilometers based on an absolute magnitude of 10.65. [7]

    Notes

    1. 1 2 Lightcurve plot of (1111) Reinmuthia, by H. & H. Hamanowa (2009) from observations at the Hamanowa Astronomical Observatory ( D91 ). Rotation period 4.0075±0.0001 hours (0.166979 days) and a brightness amplitude of 0.945±0.005 mag. Summary figures at the LCDB

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    References

    1. 1 2 3 4 5 6 7 8 9 "JPL Small-Body Database Browser: 1111 Reinmuthia (1927 CO)" (2017-11-02 last obs.). Jet Propulsion Laboratory . Retrieved 26 January 2018.
    2. 1 2 3 Schmadel, Lutz D. (2007). "(1111) Reinmuthia". Dictionary of Minor Planet Names. Springer Berlin Heidelberg. p. 94. doi:10.1007/978-3-540-29925-7_1112. ISBN   978-3-540-00238-3.
    3. 1 2 3 "1111 Reinmuthia (1927 CO)". Minor Planet Center. Retrieved 26 January 2018.
    4. 1 2 "Asteroid 1111 Reinmuthia – Proper Elements". AstDyS-2, Asteroids – Dynamic Site. Retrieved 13 March 2020.
    5. 1 2 3 4 "Asteroid 1111 Reinmuthia". Small Bodies Data Ferret. Retrieved 13 March 2020.
    6. 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". Publications of the Astronomical Society of Japan. 63 (5): 1117–1138. Bibcode:2011PASJ...63.1117U. doi: 10.1093/pasj/63.5.1117 . (online, AcuA catalog p. 153)
    7. 1 2 3 4 5 6 7 "LCDB Data for (1111) Reinmuthia". Asteroid Lightcurve Database (LCDB). Retrieved 26 January 2018.
    8. 1 2 3 Behrend, Raoul. "Asteroids and comets rotation curves – (1111) Reinmuthia". Geneva Observatory . Retrieved 26 January 2018.
    9. 1 2 Hanuš, J.; Ďurech, J.; Brož, M.; Marciniak, A.; Warner, B. D.; Pilcher, F.; et al. (March 2013). "Asteroids' physical models from combined dense and sparse photometry and scaling of the YORP effect by the observed obliquity distribution". Astronomy and Astrophysics. 551: A67. arXiv: 1301.6943 . Bibcode:2013A&A...551A..67H. doi:10.1051/0004-6361/201220701. ISSN   0004-6361.
    10. 1 2 Hamanowa, Hiromi; Hamanowa, Hiroko (July 2009). "Lightcurves of 494 Virtus, 556 Phyllis, 624 Hektor 657 Gunlod, 111 Reinmuthia, 1188 Gothlandia, and 1376 Michelle" (PDF). Minor Planet Bulletin. 36 (3): 87–88. Bibcode:2009MPBu...36...87H. ISSN   1052-8091. Archived from the original (PDF) on 26 November 2021. Retrieved 13 March 2020.
    11. 1 2 3 Binzel, R. P. (October 1987). "A photoelectric survey of 130 asteroids". Icarus: 135–208. Bibcode:1987Icar...72..135B. doi:10.1016/0019-1035(87)90125-4. ISSN   0019-1035 . Retrieved 26 January 2018.
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