Astronomy:1153 Wallenbergia
| Discovery[1] | |
|---|---|
| Discovered by | S. Belyavskyj |
| Discovery site | Simeiz Obs. |
| Discovery date | 5 September 1924 |
| Designations | |
| (1153) Wallenbergia | |
| Named after | Georg Wallenberg[2][lower-alpha 1] (German mathematician) |
| 1924 SL · 1930 HH | |
| Minor planet category | main-belt · (inner) · Flora[3] |
| Orbital characteristics[1] | |
| Epoch 4 September 2017 (JD 2458000.5) | |
| Uncertainty parameter 0 | |
| Observation arc | 87.02 yr (31,784 days) |
| |{{{apsis}}}|helion}} | 2.5489 AU |
| |{{{apsis}}}|helion}} | 1.8428 AU |
| 2.1958 AU | |
| Eccentricity | 0.1608 |
| Orbital period | 3.25 yr (1,189 days) |
| Mean anomaly | 237.52° |
| Mean motion | 0° 18m 10.44s / day |
| Inclination | 3.3345° |
| Longitude of ascending node | 280.54° |
| 28.766° | |
| Physical characteristics | |
| Dimensions | 8.02±1.81 km[4] 8.037±0.357 km[5] 9.36 km (derived)[3] |
| Rotation period | 4.096±0.002 h[6] 4.116±0.0055 h[7] 4.12±0.070 h[8] |
| Geometric albedo | 0.24 (assumed)[3] 0.37±0.14[4] 0.433±0.091[5] |
| S[3][9] | |
| Absolute magnitude (H) | 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] |
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]
Orbit and classification
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 characteristics
Wallenbergia has been characterized as a stony S-type asteroid by PanSTARRS photometric survey.[9]
Rotation period
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 ({{{1}}}).[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 ({{{1}}}).[7][8]
Diameter and albedo
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]
Naming
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][lower-alpha 1]
Notes
References
- ↑ 1.0 1.1 1.2 1.3 "JPL Small-Body Database Browser: 1153 Wallenbergia (1924 SL)". Jet Propulsion Laboratory. https://ssd.jpl.nasa.gov/sbdb.cgi?sstr=2001153. Retrieved 8 September 2017.
- ↑ 2.0 2.1 2.2 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.
- ↑ 3.0 3.1 3.2 3.3 3.4 3.5 3.6 "LCDB Data for (1153) Wallenbergia". Asteroid Lightcurve Database (LCDB). http://www.minorplanet.info/PHP/generateOneAsteroidInfo.php?AstInfo=1153%7CWallenbergia. Retrieved 8 September 2017.
- ↑ 4.0 4.1 4.2 4.3 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. doi:10.3847/0004-6256/152/3/63. Bibcode: 2016AJ....152...63N.
- ↑ 5.0 5.1 5.2 5.3 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. doi:10.1088/2041-8205/759/1/L8. Bibcode: 2012ApJ...759L...8M. http://adsabs.harvard.edu/cgi-bin/bib_query?bibcode=2012ApJ...759L...8M. Retrieved 8 September 2017.
- ↑ 6.0 6.1 6.2 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. http://adsabs.harvard.edu/cgi-bin/bib_query?bibcode=1995LPI....26.1511W. Retrieved 8 September 2017.
- ↑ 7.0 7.1 7.2 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. doi:10.1088/0004-6256/150/3/75. Bibcode: 2015AJ....150...75W. http://adsabs.harvard.edu/cgi-bin/bib_query?bibcode=2015AJ....150...75W. Retrieved 8 September 2017.
- ↑ 8.0 8.1 8.2 Chang, Chan-Kao (August 2015). "Asteroid Spin-rate Study Using the Intermediate Palomar Transient Factory". The Astrophysical Journal Supplement Series 219 (2): 19. doi:10.1088/0067-0049/219/2/27. Bibcode: 2015ApJS..219...27C. http://adsabs.harvard.edu/cgi-bin/bib_query?bibcode=2015ApJS..219...27C. Retrieved 8 September 2017.
- ↑ 9.0 9.1 9.2 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. doi:10.1016/j.icarus.2015.08.007. Bibcode: 2015Icar..261...34V. http://adsabs.harvard.edu/cgi-bin/bib_query?bibcode=2015Icar..261...34V. Retrieved 8 September 2017.
- ↑ 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. doi:10.1016/j.icarus.2012.07.026. Bibcode: 2012Icar..221..365P. http://adsabs.harvard.edu/cgi-bin/bib_query?bibcode=2012Icar..221..365P. Retrieved 8 September 2017.
- ↑ 11.0 11.1 "1153 Wallenbergia (1924 SL)". Minor Planet Center. https://www.minorplanetcenter.net/db_search/show_object?object_id=1153. Retrieved 8 September 2017.
External links
- Theorie der linearen Differenzengleichungen, by Georg Wallenberg, Alf Guldberg
- Asteroid Lightcurve Database (LCDB), query form (info )
- Dictionary of Minor Planet Names, Google books
- Asteroids and comets rotation curves, CdR – Observatoire de Genève, Raoul Behrend
- Discovery Circumstances: Numbered Minor Planets (1)-(5000) – Minor Planet Center
- 1153 Wallenbergia at AstDyS-2, Asteroids—Dynamic Site
- 1153 Wallenbergia at the JPL Small-Body Database
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