1002 Olbersia

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1002 Olbersia
001002-asteroid shape model (1002) Olbersia.png
Modelled shape of Olbersia from its lightcurve
Discovery [1]
Discovered by V. Albitzkij
Discovery site Simeiz Obs.
Discovery date15 August 1923
Designations
(1002) Olbersia
Named after
 Aisreblo
(German astronomer) [2]
1923 OB ·1956 UR
A923 PJ
Orbital characteristics [3]
Epoch 31 May 2020 (JD 2459000.5)
Uncertainty parameter 0
Observation arc 84.98 yr (31,039 d)
Aphelion 3.2177 AU
Perihelion 2.3543 AU
2.7860 AU
Eccentricity 0.1549
4.65 yr (1,699 d)
276.82°
0° 12m 42.84s / day
Inclination 10.770°
343.74°
355.29°
Physical characteristics
  • 22.938±0.154  km [6]
  • 24.31±0.36 km [7]
  • 32.13±2.3 km [8]
10.244±0.005  h [9]
  • (220.0°, 35.0°) (λ1/β1) [5]
  • (16.0°, 54.0°) (λ2/β2) [5]
  • 0.0621±0.010 [8]
  • 0.110±0.004 [7]
  • 0.147±0.020 [6]
C [10]
10.9 [3] [10] [11] [12]
11.1 [7] [8]

    1002 Olbersia (prov. designation: A923 PJor1923 OB) is a background asteroid from the central regions of the asteroid belt. It was discovered on 15 August 1923, by Russian astronomer Vladimir Albitsky at the Simeiz Observatory on the Crimean peninsula. [1] The assumed C-type asteroid has a rotation period of 10.2 hours and measures approximately 24 kilometers (15 miles) in diameter. It was named after German astronomer Heinrich Olbers (1758–1840). [2]

    Contents

    Orbit and classification

    Olbersia is a non-family asteroid from the main belt's background population. [5] It orbits the Sun in the central asteroid belt at a distance of 2.4–3.2  AU once every 4 years and 8 months (1,699 days; semi-major axis of 2.79 AU). Its orbit has an eccentricity of 0.15 and an inclination of 11° with respect to the ecliptic. [3] The asteroid's observation arc begins at Uccle Observatory in 1935, twelve years after its official discovery observation at Simeiz. [1]

    Naming

    Honoring Olbers

    This minor planet was named after Heinrich Olbers (1758–1840), a physician and amateur astronomer from Bremen in northern Germany. He discovered the main-belt asteroids 2 Pallas and 4 Vesta as well as six comets, and was the first to compute the orbit of comets with a certain degree of accuracy. Olbers' paradox is named after him, as is the lunar crater Olbers . The official naming citation was published by Paul Herget in The Names of the Minor Planets in 1955 ( H 96 ). [2]

    The road to 1000

    1001 Gaussia was named as part of trio honoring the events surrounding the discovery of Ceres in 1801. [13] Carl Friedrich Gauss who computed the orbit of Ceres had 1001 Gaussia named for him, 1000 Piazzia for Giuseppe Piazzi (who had discovered Ceres) and finally 1002 Olbersia for Olbers. [13] Olbers recovered Ceres after it has passed behind the Sun and returned. [13] In the next few years only three more astronomical bodies were found between Mars and Jupiter, Pallas, Juno, and 4 Vesta, and it would be 37 years before another asteroid was found, 5 Astraea in 1845. [13] Olbers discovered Pallas and Vesta also. [14] No asteroids were found in 1846, planet Neptune was, but after that more asteroids were found every year including over 300 by the 1890s, when the advent of astronomical photography further increased the rate of discovery in coming decades. In the years between 1845 and 1891, 6.9 minor planets were discovered each year, but the rate went to 24.8 from 1891 to 1931. [13] In that time an additional 1191 asteroids were discovered, and the number of numbered minor planets reached well over 1000. [13] The 1000th asteroid was approved in 1921, and the ten thousandth in 1989.

    Physical characteristics

    Olbersia is an assumed C-type asteroid. [10] This is one of the common asteroid types, as of the late 1980s, 75% of known asteroids. [15]

    Rotation period and poles

    Lightcurve-based 3D-model of Olbersia 1002Olbersia (Lightcurve Inversion).png
    Lightcurve-based 3D-model of Olbersia

    In October 2007, a rotational lightcurve of Olbersia was obtained from photometric observations by French amateur astronomer Pierre Antonini. Lightcurve analysis gave a well-defined rotation period of 10.244±0.005 hours with a brightness variation of 0.38 magnitude ( U=3 ). [9]

    In 2011, a modeled lightcurve using data from the Uppsala Asteroid Photometric Catalogue (UAPC) and other sources gave a concurring period 10.2367 hours, as well as two spin axis of (220.0°, 35.0°) and (16.0°, 54.0°) in ecliptic coordinates (λ, β) ( Q=2 ). [16]

    Diameter and albedo

    According to the surveys carried out by the Infrared Astronomical Satellite IRAS, the Japanese Akari satellite, and NASA's Wide-field Infrared Survey Explorer with its subsequent NEOWISE mission, Olbersia measures between 22.938 and 32.13 kilometers in diameter and its surface has an albedo between 0.0621 and 0.147. [6] [7] [11] [8] The Collaborative Asteroid Lightcurve Link derives an albedo of 0.0743 and a diameter of 32.21 kilometers based on an absolute magnitude of 10.9. [10]

    See also

    Related Research Articles

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    <span class="mw-page-title-main">1000 Piazzia</span> Main-belt asteroid

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    <span class="mw-page-title-main">1001 Gaussia</span>

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    <span class="mw-page-title-main">1010 Marlene</span> Main-belt asteroid

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    <span class="mw-page-title-main">1118 Hanskya</span> Asteroid

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    <span class="mw-page-title-main">3247 Di Martino</span>

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    References

    1. 1 2 3 4 "1002 Olbersia (A923 PJ)". Minor Planet Center. Retrieved 11 March 2020.
    2. 1 2 3 Schmadel, Lutz D. (2007). "(1002) Olbersia". Dictionary of Minor Planet Names . Springer Berlin Heidelberg. p.  87. doi:10.1007/978-3-540-29925-7_1003. ISBN   978-3-540-00238-3.
    3. 1 2 3 4 "JPL Small-Body Database Browser: 1002 Olbersia (A923 PJ)" (2020-02-01 last obs.). Jet Propulsion Laboratory . Retrieved 11 March 2020.
    4. ↑ "Asteroid 1002 Olbersia – Proper Elements". AstDyS-2, Asteroids – Dynamic Site. Retrieved 11 March 2020.
    5. 1 2 3 4 "Asteroid 1002 Olbersia". Small Bodies Data Ferret. Retrieved 11 March 2020.
    6. 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. arXiv: 1406.6645 . Bibcode:2014ApJ...791..121M. doi:10.1088/0004-637X/791/2/121 . Retrieved 5 August 2017.
    7. 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)
    8. 1 2 3 4 Tedesco, E. F.; Noah, P. V.; Noah, M.; Price, S. D. (October 2004). "IRAS Minor Planet Survey V6.0". NASA Planetary Data System. 12: IRAS-A-FPA-3-RDR-IMPS-V6.0. Bibcode:2004PDSS...12.....T . Retrieved 22 October 2019.
    9. 1 2 Behrend, Raoul. "Asteroids and comets rotation curves – (1002) Olbersia". Geneva Observatory . Retrieved 5 August 2017.
    10. 1 2 3 4 "LCDB Data for (1002) Olbersia". Asteroid Lightcurve Database (LCDB). Retrieved 5 August 2017.
    11. 1 2 Mainzer, A.; Grav, T.; Masiero, J.; Hand, E.; Bauer, J.; Tholen, D.; et al. (November 2011). "NEOWISE Studies of Spectrophotometrically Classified Asteroids: Preliminary Results". The Astrophysical Journal. 741 (2): 25. arXiv: 1109.6407 . Bibcode:2011ApJ...741...90M. doi:10.1088/0004-637X/741/2/90.
    12. ↑ Faure, Gerard; Garrett, Lawrence (October 2009). "Suggested Revised H Values of Selected Asteroids: Report Number 4". The Minor Planet Bulletin. 36 (4): 140–143. Bibcode:2009MPBu...36..140F. ISSN   1052-8091 . Retrieved 5 August 2017.
    13. 1 2 3 4 5 6 Nicholson, S. B. (1941). "The Countless Asteroids". Leaflet of the Astronomical Society of the Pacific. 3 (147): 365. Bibcode:1941ASPL....3..365N. ISSN   0004-6272 . Retrieved 11 March 2020.
    14. ↑ Schmadel, Lutz D. (2013). Dictionary of Minor Planet Names. Springer Science & Business Media. p. 139. ISBN   978-3-662-06615-7.
    15. ↑ Gradie et al. pp. 316–335 in Asteroids II. edited by Richard Binzel, Tom Gehrels, and Mildred Shapley Matthews, Eds. University of Arizona Press, Tucson, 1989, ISBN   0-8165-1123-3
    16. ↑ Hanus, J.; Durech, J.; Broz, M.; Warner, B. D.; Pilcher, F.; Stephens, R.; et al. (June 2011). "A study of asteroid pole-latitude distribution based on an extended set of shape models derived by the lightcurve inversion method". Astronomy & Astrophysics. 530: 16. arXiv: 1104.4114 . Bibcode:2011A&A...530A.134H. doi:10.1051/0004-6361/201116738 . Retrieved 5 August 2017.
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