1259 Ógyalla

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1259 Ógyalla
Discovery [1]
Discovered by K. Reinmuth
Discovery site Heidelberg Obs.
Discovery date 29 January 1933
MPC designation (1259) Ógyalla
Named after
Hurbanovo Observatory (551)
(formerly O'Gyalla Observatory)[2]
1933 BT · 1928 DJ1
1928 FO · 1929 MA
1935 QE1 · 1949 YN
1956 JF
main-belt · Themis[3][4]
Orbital characteristics[1]
Epoch 4 September 2017 (JD 2458000.5)
Uncertainty parameter 0
Observation arc 89.36 yr (32,640 days)
Aphelion 3.5000 AU
Perihelion 2.7064 AU
3.1032 AU
Eccentricity 0.1279
5.47 yr (1,997 days)
0° 10m 49.08s / day
Inclination 2.3810°
Physical characteristics
Dimensions 26.59±7.87 km[5]
31.32±1.13 km[6]
33.13±1.6 km[7]
33.31 km (derived)[3]
36.111±0.510 km[8]
39.484±0.440 km[9]
12 h (dated)[10]
17.2669±0.1183 h (S)[11]
17.3038±0.0573 h (R)[11]
17.334±0.004 h[12]
0.0916 (derived)[3]
10.349±0.002 (R)[11] · 10.6[1][3] · 10.64[5] · 10.678±0.003 (S)[11] · 11.0[6][7][9]

1259 Ógyalla, provisional designation 1933 BT, is a Themistian asteroid from the outer region of the asteroid belt, approximately 32 kilometers in diameter. It was discovered on 29 January 1933, by German astronomer Karl Reinmuth at Heidelberg Observatory in southwest Germany.[13] The asteroid was named for the Hurbanovo Observatory (551).[2]

Orbit and classification[edit]

Ógyalla is a member of the Themis family, the 9th largest main-belt asteroid family of nearly 5,000 asteroids with nearly coplanar ecliptical orbits.[4] It orbits the Sun in the outer main-belt at a distance of 2.7–3.5 AU once every 5 years and 6 months (1,997 days). Its orbit has an eccentricity of 0.13 and an inclination of 2° with respect to the ecliptic.[1] It was first identified as 1928 DJ1 and 1928 FO at the discovering observatory in 1928, extending the asteroid's observation arc by 5 years prior to its official discovery observation.[13]

Physical characteristics[edit]

Rotation period[edit]

A rotational lightcurve of Ógyalla was obtained by the Spanish Photometric Asteroid Analysis Group (OBAS) in June 2016. Light curve analysis gave a well-defined rotation period of 17.334 hours with a brightness variation of 0.41 magnitude (U=3).[12] In September 2012, photometric observations at the Palomar Transient Factory gave a period of 17.2669 and 17.3038 hours with an amplitude of 0.27 and 0.25 in the R- and S-band, respectively (U=2/2).[11]

The first lightcurve was already obtained in 1974, by Swedish astronomer Claes-Ingvar Lagerkvist at Uppsala Observatory from photographic photometry, but it was only fragmentary and gave a tentative period of 12 hours (U=1).[10]

Diameter and albedo[edit]

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, Ógyalla measures between 26.59 and 36.11 kilometers in diameter, and its surface has an albedo between 0.064 and 0.10 (without preliminary results).[5][6][7][8] The Collaborative Asteroid Lightcurve Link (CALL) derives an albedo of 0.0916 and a diameter of 33.31 kilometers based on an absolute magnitude of 10.6. CALL also classifies it as a stony S-type asteroid (as it does with all Themistians).[3]


This minor planet was named for the Hurbanovo Observatory (IAU code: 551; formerly known as O'Gyalla Observatory), a seismological, meteorological and astronomical observatory in the former Hungarian city of Ógyalla. Since 1948, the city belongs to Slovakia and is now known as Hurbanovo.[2] The official naming citation was mentioned in The Names of the Minor Planets by Paul Herget in 1955 (H 116).[2]


  1. ^ a b c d "JPL Small-Body Database Browser: 1259 Ogyalla (1933 BT)" (2017-07-05 last obs.). Jet Propulsion Laboratory. Retrieved 26 July 2017. 
  2. ^ a b c d Schmadel, Lutz D. (2007). Dictionary of Minor Planet Names – (1259) Ógyalla. Springer Berlin Heidelberg. p. 104. ISBN 978-3-540-00238-3. Retrieved 24 January 2017. 
  3. ^ a b c d e f "LCDB Data for (1259) Ógyalla". Asteroid Lightcurve Database (LCDB). Retrieved 24 January 2017. 
  4. ^ a b Alvarez-Candal, Alvaro; Duffard, René; Angeli, Cláudia A.; Lazzaro, Daniela; Fernández, Silvia (December 2004). "Rotational lightcurves of asteroids belonging to families". Icarus. 172 (2): 388–401. Bibcode:2004Icar..172..388A. doi:10.1016/j.icarus.2004.06.008. Retrieved 22 November 2015. 
  5. ^ 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:1606.08923Freely accessible. Bibcode:2016AJ....152...63N. doi:10.3847/0004-6256/152/3/63. Retrieved 24 January 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 24 January 2017. 
  7. ^ a b c d Tedesco, E. F.; Noah, P. V.; Noah, M.; Price, S. D. (October 2004). "IRAS Minor Planet Survey V6.0". NASA Planetary Data System. Bibcode:2004PDSS...12.....T. Retrieved 24 January 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 24 January 2017. 
  9. ^ a b c 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 24 January 2017. 
  10. ^ a b Lagerkvist, C.-I. (March 1978). "Photographic photometry of 110 main-belt asteroids". Astronomy and Astrophysics Supplement Series: 361–381. Bibcode:1978A&AS...31..361L. Retrieved 24 January 2017. 
  11. ^ a b c d e 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:1504.04041Freely accessible. Bibcode:2015AJ....150...75W. doi:10.1088/0004-6256/150/3/75. Retrieved 24 January 2017. 
  12. ^ a b Mansego, Enrique Arce; Rodriguez, Pedro Brines; de Haro, Juan Lozano; Chiner, Onofre Rodrigo; Silva, Alvaro Fornas; Porta, David Herrero; et al. (October 2016). "Eighteen Asteroids Lightcurves at Asteroides Observers (OBAS) - MPPD: 2016 March-May". The Minor Planet Bulletin. 43 (4): 332–336. Bibcode:2016MPBu...43..332M. ISSN 1052-8091. Retrieved 24 January 2017. 
  13. ^ a b "1259 Ogyalla (1933 BT)". Minor Planet Center. Retrieved 24 January 2017. 

External links[edit]