1372 Haremari

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1372 Haremari
Discovery [1]
Discovered by K. Reinmuth
Discovery site Heidelberg Obs.
Discovery date 31 August 1935
Designations
MPC designation (1372) Haremari
Named after
all female staff members of ARI[2]
1935 QK · 1928 DX
1937 BD · 1944 QK
1951 EW1 · 1953 OM
1953 PZ
main-belt · (middle)
Watsonia[3] · Ceres trojan [4]
Orbital characteristics[1]
Epoch 4 September 2017 (JD 2458000.5)
Uncertainty parameter 0
Observation arc 89.18 yr (32,574 days)
Aphelion 3.1761 AU
Perihelion 2.3557 AU
2.7659 AU
Eccentricity 0.1483
4.60 yr (1,680 days)
243.89°
0° 12m 51.48s / day
Inclination 16.450°
327.45°
88.484°
Physical characteristics
Dimensions 21.96±0.72 km[5]
23.90±0.53 km[6]
24.18 km (derived)[7]
26.491±0.292 km[8]
27.724±0.158 km[9]
31.17±8.52 km[10]
15.25±0.03 h[11]
0.0303±0.0021[9]
0.039±0.012[8]
0.09±0.03[10]
0.1097 (derived)[7]
0.126±0.006[6]
0.146±0.027[5]
SMASS = L[1][7]
11.00[5][6][10] · 11.1[1][7] · 12.2[9]

1372 Haremari, provisional designation 1935 QK, is a rare-type Watsonian asteroid and a suspected trojan of Ceres from the central regions of the asteroid belt, approximately 26 kilometers in diameter. It was discovered on 31 August 1935, by astronomer Karl Reinmuth at the Heidelberg-Königstuhl State Observatory in southwest Germany.[12] The asteroid was named for all female staff members of the Astronomical Calculation Institute.[2]

Orbit and classification[edit]

Haremari is a member of the very small Watsonia family (537), named after its parent body, namesake and largest member, 729 Watsonia.[3][13]:23

It orbits the Sun in the central main-belt at a distance of 2.4–3.2 AU once every 4 years and 7 months (1,680 days). Its orbit has an eccentricity of 0.15 and an inclination of 16° with respect to the ecliptic.[1] The body's observation arc begins with its first observation at Heidelberg in February 1928, more than seven years prior to its official discovery observation.[12]

Trojan of Ceres[edit]

Long-term numerical integrations suggest, that Haremari is a trojan of Ceres, staying a 1:1 orbital resonance with the only dwarf planet of the asteroid belt. It is thought that Haremari is currently transiting from a tadpole to a horseshoe orbit. Other suspected co-orbitals are the asteroids 855 Newcombia, 4608 Wodehouse and 8877 Rentaro.[4][14]

Physical characteristics[edit]

In the SMASS classification, Haremari is a rare L-type asteroid with a moderate albedo.[1][7] This type corresponds with the overall spectral type of the Watsonia family.[13]:23

Rotation period[edit]

In November 2009, a rotational lightcurve of Haremari was obtained from photometric observations by Richard Durkee at the Shed of Science Observatory (H39). Lightcurve analysis gave a rotation period of 15.25 hours with a brightness amplitude of 0.12 magnitude (U=2).[11]

Diameter and albedo[edit]

According to the surveys carried out by the Japanese Akari satellite and the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer, Haremari measures between 21.96 and 31.17 kilometers in diameter and its surface has an albedo between 0.0303 and 0.146.[5][6][8][9][10]

The Collaborative Asteroid Lightcurve Link derives an albedo of 0.1097 and a diameter of 24.18 kilometers based on an absolute magnitude of 11.1.[7]

Naming[edit]

This minor planet jointly honors all the female staff members of the Astronomical Calculation Institute (Heidelberg University) (German: Astronomisches Rechen-Institut), commonly known as ARI. In often published versions, "Haremari" is a composed name and means "the harem of A.R.I.".[2]

Alternative version[edit]

According to Ingrid van Houten-Groeneveld, who worked as a young astronomer at Heidelberg, Reinmuth had often been asked by his colleges at ARI to name some of his discoveries after their female friends, as wells as after popular actresses (and not just the female staff at ARI). He then compiled all these proposals to the name "Haremari". However, as Groeneveld recorded, "Reinmuth did not want to publish the original meaning and he, therefore, devised the interpretation of the first sentence in 1948".[2]

References[edit]

  1. ^ a b c d e f "JPL Small-Body Database Browser: 1372 Haremari (1935 QK)" (2017-05-04 last obs.). Jet Propulsion Laboratory. Retrieved 31 October 2017. 
  2. ^ a b c d Schmadel, Lutz D. (2007). Dictionary of Minor Planet Names – (1372) Haremari. Springer Berlin Heidelberg. p. 111. ISBN 978-3-540-00238-3. Retrieved 31 October 2017. 
  3. ^ a b "Small Bodies Data Ferret". Nesvorny HCM Asteroid Families V3.0. Retrieved 31 October 2017. 
  4. ^ a b Christou, A. A. (April 2000). "Co-orbital objects in the main asteroid belt". Astronomy and Astrophysics: L71–L74. Bibcode:2000A&A...356L..71C. Retrieved 31 October 2017. 
  5. ^ a b c d Masiero, Joseph R.; Mainzer, A. K.; Grav, T.; Bauer, J. M.; Cutri, R. M.; Nugent, C.; et al. (November 2012). "Preliminary Analysis of WISE/NEOWISE 3-Band Cryogenic and Post-cryogenic Observations of Main Belt Asteroids". The Astrophysical Journal Letters. 759 (1): 5. arXiv:1209.5794Freely accessible. Bibcode:2012ApJ...759L...8M. doi:10.1088/2041-8205/759/1/L8. Retrieved 31 October 2017. 
  6. ^ a b c d 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. Retrieved 31 October 2017. 
  7. ^ a b c d e f "LCDB Data for (1372) Haremari". Asteroid Lightcurve Database (LCDB). Retrieved 31 October 2017. 
  8. ^ a b c 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:1406.6645Freely accessible. Bibcode:2014ApJ...791..121M. doi:10.1088/0004-637X/791/2/121. Retrieved 31 October 2017. 
  9. ^ a b c d 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. arXiv:1109.6407Freely accessible. Bibcode:2011ApJ...741...90M. doi:10.1088/0004-637X/741/2/90. Retrieved 31 October 2017. 
  10. ^ a b c d 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:1509.02522Freely accessible. Bibcode:2015ApJ...814..117N. doi:10.1088/0004-637X/814/2/117. Retrieved 31 October 2017. 
  11. ^ a b Durkee, Russell I. (July 2010). "Asteroids Observed from the Shed of Science Observatory: 2009 October - 2010 March". The Minor Planet Bulletin. 37 (3): 125–127. Bibcode:2010MPBu...37..125D. ISSN 1052-8091. Retrieved 31 October 2017. 
  12. ^ a b "1372 Haremari (1935 QK)". Minor Planet Center. Retrieved 31 October 2017. 
  13. ^ a b Nesvorný, D.; Broz, M.; Carruba, V. (December 2014). "Identification and Dynamical Properties of Asteroid Families" (PDF). Asteroids IV: 297–321. arXiv:1502.01628Freely accessible. Bibcode:2015aste.book..297N. doi:10.2458/azu_uapress_9780816532131-ch016. Retrieved 31 October 2017. 
  14. ^ Christou, A. (November 2001). "The Trojans of Ceres and Vesta". American Astronomical Society. 33: 1134. Bibcode:2001DPS....33.5205C. Retrieved 31 October 2017. 

External links[edit]