Astronomy:834 Burnhamia

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834 Burnhamia
000834-asteroid shape model (834) Burnhamia.png
Shape of Burnhamia from modeled lightcurve
Discovery [1]
Discovered byM. F. Wolf
Discovery siteHeidelberg Obs.
Discovery date20 September 1916
Designations
(834) Burnhamia
Pronunciation/bərnˈheɪmiə/
Named afterSherburne Wesley Burnham
(American astronomer)[2]
A916 SG · 1959 CA
1972 JE · A905 UM
1916 AD · 1905 UM
Minor planet category
Orbital characteristics [3]
Epoch 31 May 2020 (JD 2459000.5)
Uncertainty parameter 0
Observation arc114.27 yr (41,737 d)
|{{{apsis}}}|helion}}3.8256 AU
|{{{apsis}}}|helion}}2.5443 AU
3.1849 AU
Eccentricity0.2012
Orbital period5.68 yr (2,076 d)
Mean anomaly207.71°
Mean motion0° 10m 24.24s / day
Inclination3.9779°
Longitude of ascending node182.68°
91.320°
Physical characteristics
Mean diameter
Rotation period13.875±0.001 h[10]
Geometric albedo
  • Tholen = GS: [3]
  • X (S3OS2)[11]
  • B–V = 0.752±0.020[3]
  • U–B = 0.472±0.047[3]
Absolute magnitude (H)9.5[1][3]


834 Burnhamia (prov. designation: A916 SG or 1916 AD) is a large background asteroid, approximately 61 kilometers (38 miles) in diameter, that is located in the outer region of the asteroid belt. It was discovered on 20 September 1916, by German astronomer Max Wolf at the Heidelberg Observatory in southwest Germany.[1] The X-type asteroid (GS) has a rotation period of 13.9 hours. It was named after American astronomer Sherburne Wesley Burnham (1838–1921).[2]

Orbit and classification

Burnhamia 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 main-belt at a distance of 2.5–3.8 AU once every 5 years and 8 months (2,076 days; semi-major axis of 3.18 AU). Its orbit has an eccentricity of 0.20 and an inclination of 4° with respect to the ecliptic.[3] The asteroid's observation arc begins with its first observation as A905 UM at Heidelberg Observatory on 26 October 1905, almost 11 years prior to its official discovery observation.[1]

Naming

This minor planet was named after Sherburne Wesley Burnham (1838–1921), American astronomer who discovered many visual binary stars and is known for his Burnham Double Star Catalogue (BDS), a catalogue of double stars seen in the Northern Hemisphere, which was published in two parts by the Carnegie Institution of Washington in 1906. Burnham observed from the Chicago (1877), Lick (1888) and Yerkes (1897) observatories. The naming was published in the journal Astronomische Nachrichten in 1921 (AN 214, 69), and was also mentioned in The Names of the Minor Planets by Paul Herget in 1955 (H 82).[2] The lunar crater Burnham is also named in his honor.[12]

Physical characteristics

In the Tholen classification, Burnhamia is closest to a G-type asteroid and somewhat similar to a common stony S-type asteroid,[3] while In ioth the Tholen- and SMASS-like taxonomy of the Small Solar System Objects Spectroscopic Survey (S3OS2), Burnhamia is an X-type asteroid.[5][11]

Rotation period

In October 2006, a rotational lightcurve of Burnhamia was obtained from photometric observations by Robert Buchheim at the Altimira Observatory (G76) in California. Lightcurve analysis gave a well-defined rotation period of 13.875±0.001 hours with a brightness variation of 0.20±0.02 magnitude ({{{1}}}).[10] The result supersedes previous observations by French amateur astronomer Laurent Bernasconi from May 2005, with a period of 13.9±0.03 hours with an amplitude of 0.15±0.01 magnitude ({{{1}}}), and from October 2006, that gave a period of 13.85±0.03 hours and an amplitude of 0.22±0.02 magnitude ({{{1}}}).[13]

Diameter and albedo

According to the surveys carried out by the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer (WISE), the Japanese Akari satellite, and the Infrared Astronomical Satellite IRAS, Burnhamia measures (61.278±0.303), (61.44±2.13) and (66.65±2.4) kilometers in diameter and its surface has an albedo of (0.071±0.008), (0.082±0.007) and (0.0698±0.005), respectively.[6][7][9][8] The Collaborative Asteroid Lightcurve Link derives an albedo of 0.0602 and a diameter of 66.64 kilometers based on an absolute magnitude of 9.55.[14] The WISE team also published an alternative mean-diameter of (66.151±1.727 km) with corresponding albedos of (0.0611±0.0082).[5][14] Two asteroid occultations of Burnhamia September 2013 and January 2014, gave both a best-fit ellipse dimension of (61.0 km × 61.0 km).[5] These timed observations are taken when the asteroid passes in front of a distant star.

References

  1. ↑ 1.0 1.1 1.2 1.3 1.4 "834 Burnhamia (A916 SG)". Minor Planet Center. https://www.minorplanetcenter.net/db_search/show_object?object_id=834. 
  2. ↑ 2.0 2.1 2.2 Schmadel, Lutz D. (2007). "(834) Burnhamia". Dictionary of Minor Planet Names. Springer Berlin Heidelberg. p. 77. doi:10.1007/978-3-540-29925-7_835. ISBN 978-3-540-00238-3. 
  3. ↑ 3.0 3.1 3.2 3.3 3.4 3.5 3.6 3.7 "JPL Small-Body Database Browser: 834 Burnhamia (A916 SG)". Jet Propulsion Laboratory. https://ssd.jpl.nasa.gov/sbdb.cgi?sstr=2000834. 
  4. ↑ 4.0 4.1 "Asteroid 834 Burnhamia – Proper Elements". AstDyS-2, Asteroids – Dynamic Site. https://newton.spacedys.com/astdys/index.php?pc=1.1.6&n=834. 
  5. ↑ 5.0 5.1 5.2 5.3 5.4 "Asteroid 834 Burnhamia". Small Bodies Data Ferret. https://sbntools.psi.edu/ferret/SimpleSearch/results.action?targetName=834+Burnhamia. 
  6. ↑ 6.0 6.1 6.2 Mainzer, A. K.; Bauer, J. M.; Cutri, R. M.; Grav, T.; Kramer, E. A.; Masiero, J. R. et al. (June 2016). "NEOWISE Diameters and Albedos V1.0". NASA Planetary Data System. Bibcode: 2016PDSS..247.....M. https://sbnarchive.psi.edu/pds3/non_mission/EAR_A_COMPIL_5_NEOWISEDIAM_V1_0/data/neowise_mainbelt.tab. Retrieved 9 March 2020. 
  7. ↑ 7.0 7.1 7.2 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. doi:10.1088/0004-637X/791/2/121. Bibcode: 2014ApJ...791..121M. 
  8. ↑ 8.0 8.1 8.2 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. doi:10.1093/pasj/63.5.1117. Bibcode: 2011PASJ...63.1117U.  (online, AcuA catalog p. 153)
  9. ↑ 9.0 9.1 9.2 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. https://sbnarchive.psi.edu/pds3/iras/IRAS_A_FPA_3_RDR_IMPS_V6_0/data/diamalb.tab. Retrieved 9 March 2020. 
  10. ↑ 10.0 10.1 Buchheim, Robert K. (September 2007). "Lightcurves of 25 Phocaea, 468 Lina, 482 Petrina 551 Ortrud, 741 Botolphia, 834 Burnhamia, 2839 Annette, and 3411 Debetencourt". Minor Planet Bulletin 34 (3): 68–71. ISSN 1052-8091. Bibcode: 2007MPBu...34...68B. http://www.minorplanet.info/MPB/issues/MPB_34-3.pdf. Retrieved 9 March 2020. 
  11. ↑ 11.0 11.1 Lazzaro, D.; Angeli, C. A.; Carvano, J. M.; Mothé-Diniz, T.; Duffard, R.; Florczak, M. (November 2004). "S3OS2: the visible spectroscopic survey of 820 asteroids". Icarus 172 (1): 179–220. doi:10.1016/j.icarus.2004.06.006. Bibcode: 2004Icar..172..179L. http://sirrah.troja.mff.cuni.cz/yarko-site/tmp/eos/NEW/spectral_type_figure/s3os2.pdf. Retrieved 9 March 2020. 
  12. ↑ "Crater Burnham". Gazetteer of Planetary Nomenclature. USGS Astrogeology Research Program.
  13. ↑ Behrend, Raoul. "Asteroids and comets rotation curves – (834) Burnhamia". Geneva Observatory. http://obswww.unige.ch/~behrend/page3cou.html#000834. 
  14. ↑ 14.0 14.1 "LCDB Data for (834) Burnhamia". Asteroid Lightcurve Database (LCDB). http://www.minorplanet.info/PHP/generateOneAsteroidInfo.php?AstInfo=834. 

External links



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