1153 Wallenbergia

1153 Wallenbergia, provisional designation 1924 SL, is a stony Florian asteroid from the inner regions of the asteroid belt, approximately 8 kilometers in diameter. It was discovered on 5 September 1924, by Soviet astronomer Sergey Belyavsky at the Simeiz Observatory on the Crimean peninsula.[11] The asteroid was named after German mathematician Georg Wallenberg.[2]

1153 Wallenbergia
Discovered byS. Belyavskyj
Discovery siteSimeiz Obs.
Discovery date5 September 1924
(1153) Wallenbergia
Named after
Georg Wallenberg[2][a]
(German mathematician)
1924 SL · 1930 HH
main-belt · (inner) · Flora[3]
Orbital characteristics[1]
Epoch 4 September 2017 (JD 2458000.5)
Uncertainty parameter 0
Observation arc87.02 yr (31,784 days)
Aphelion2.5489 AU
Perihelion1.8428 AU
2.1958 AU
3.25 yr (1,189 days)
0° 18m 10.44s / day
Physical characteristics
Dimensions8.02±1.81 km[4]
8.037±0.357 km[5]
9.36 km (derived)[3]
4.096±0.002 h[6]
4.116±0.0055 h[7]
4.12±0.070 h[8]
0.24 (assumed)[3]
11.985±0.002 (R)[7] · 12.00[5] · 12.040±0.100 (R)[8] · 12.1[1] · 12.28[4] · 12.31±0.08[3][6][10] · 12.49±0.22[9]

Orbit and classificationEdit

Wallenbergia is a member of the Flora family (402), a giant asteroid family and the largest family of stony asteroids in the main-belt.[3] It orbits the Sun in the inner main-belt at a distance of 1.8–2.5 AU once every 3 years and 3 months (1,189 days). Its orbit has an eccentricity of 0.16 and an inclination of 3° with respect to the ecliptic.[1]

The body's observation arc begins with its identification as 1930 HH at Johannesburg Observatory in April 1930, almost six years after its official discovery observation at Simeiz.[11]

Physical characteristicsEdit

Wallenbergia has been characterized as a stony S-type asteroid by PanSTARRS photometric survey.[9]

Rotation periodEdit

In September 1989, the first rotational lightcurve of Wallenbergia was obtained from photometric observations by Polish astronomer Wiesław Z. Wiśniewski at University of Arizona. Lightcurve analysis gave a well-defined rotation period of 4.096 hours with a brightness amplitude of 0.33 magnitude (U=3).[6] Observations in the R-band at the Palomar Transient Factory in 2014, gave a period of 4.116 and 4.12 hours with an amplitude of 0.25 and 0.23 magnitude, respectively (U=2/2).[7][8]

Diameter and albedoEdit

According to the survey carried out by the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer, Wallenbergia measures 8.02 and 8.037 kilometers in diameter and its surface has an albedo of 0.37 and 0.433, respectively.[4][5]

The Collaborative Asteroid Lightcurve Link assumes an albedo of 0.24 – taken from 8 Flora, the parent body of the Flora family – and derives a diameter of 9.36 kilometers based on an absolute magnitude of 12.31.[3]


This minor planet was named after German mathematician Georg Wallenberg (1864–1924). The official naming citation was mentioned in The Names of the Minor Planets by Paul Herget in 1955 (H 107).[2][a]


  1. ^ a b Wallenberg's middle name is likely "Jakob", not "James" as given in the Dictionary of Minor Planet Names


  1. ^ a b c d "JPL Small-Body Database Browser: 1153 Wallenbergia (1924 SL)" (2017-05-06 last obs.). Jet Propulsion Laboratory. Retrieved 8 September 2017.
  2. ^ a b c Schmadel, Lutz D. (2007). "(1153) Wallenbergia". Dictionary of Minor Planet Names – (1153) Wallenbergia. Springer Berlin Heidelberg. p. 97. doi:10.1007/978-3-540-29925-7_1154. ISBN 978-3-540-00238-3.
  3. ^ a b c d e f g "LCDB Data for (1153) Wallenbergia". Asteroid Lightcurve Database (LCDB). Retrieved 8 September 2017.
  4. ^ a b c d 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. Retrieved 8 September 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:1209.5794. Bibcode:2012ApJ...759L...8M. doi:10.1088/2041-8205/759/1/L8. Retrieved 8 September 2017.
  6. ^ a b c Wisniewski, W. Z.; Michalowski, T. M.; Harris, A. W.; McMillan, R. S. (March 1995). "Photoelectric Observations of 125 Asteroids". Abstracts of the Lunar and Planetary Science Conference. 26: 1511. Bibcode:1995LPI....26.1511W. Retrieved 8 September 2017.
  7. ^ a b c 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.
  8. ^ a b c 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. arXiv:1506.08493. Bibcode:2015ApJS..219...27C. doi:10.1088/0067-0049/219/2/27. Retrieved 8 September 2017.
  9. ^ a b c 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.
  10. ^ Pravec, Petr; Harris, Alan W.; Kusnirák, Peter; Galád, Adrián; Hornoch, Kamil (September 2012). "Absolute magnitudes of asteroids and a revision of asteroid albedo estimates from WISE thermal observations". Icarus. 221 (1): 365–387. Bibcode:2012Icar..221..365P. doi:10.1016/j.icarus.2012.07.026. Retrieved 8 September 2017.
  11. ^ a b "1153 Wallenbergia (1924 SL)". Minor Planet Center. Retrieved 8 September 2017.

External linksEdit