Astronomy:744 Aguntina

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744 Aguntina
000744-asteroid shape model (744) Aguntina.png
Modelled shape of Aguntina from its lightcurve
Discovery [1]
Discovered byJ. Rheden
Discovery siteVienna Observatory
Discovery date26 February 1913
Designations
(744) Aguntina
Pronunciation/æɡənˈtaɪnə/
Named afterAguntum
(ancient Roman town)[2]
1913 QW · 1930 DZ
1950 TL4
Minor planet categorymain-belt · (outer) [3]
Orbital characteristics [1]
Epoch 31 July 2016 (JD 2457600.5)
Uncertainty parameter 0
Observation arc103.00 yr (37621 d)
|{{{apsis}}}|helion}}3.5453 astronomical unit|AU (530.37 Gm)
|{{{apsis}}}|helion}}2.7953 AU (418.17 Gm)
3.1703 AU (474.27 Gm)
Eccentricity0.11829
Orbital period5.64 yr (2061.8 d)
Mean anomaly87.239°
Mean motion0° 10m 28.56s / day
Inclination7.7161°
Longitude of ascending node142.67°
28.637°
Earth MOID1.80382 AU (269.848 Gm)
Jupiter MOID1.44051 AU (215.497 Gm)
TJupiter3.177
Physical characteristics
Dimensions58.69±7.0 km (IRAS:25)[4]
55.80±0.86 km[5]
60.821±1.218 km[6]
68.52±3.88 km[7]
Mean radius29.345±3.5 km
Rotation period17.47±0.05 h[8]
17.5020±0.0544 h[9]
17.47 h (0.728 d)[1]
Geometric albedo0.0423±0.012 (IRAS:25)[1][4]
0.048±0.002[5]
0.0394±0.0087[6]
0.031±0.006[7]
B–V = 0.657
U–B = 0.161
Tholen = FX:
F [3]
Absolute magnitude (H)10.21[1]


744 Aguntina, provisional designation 1913 QW, is a rare-type carbonaceous asteroid from the outer region of the asteroid belt, about 60 kilometers in diameter. It was discovered by Austrian astronomer Joseph Rheden at Vienna Observatory, Austria, on 26 February 1913.[10]

The dark F-type asteroid, classified as a FX-subtype in the Tholen taxonomic scheme, orbits the Sun at a distance of 2.8–3.5 AU once every 5 years and 8 months (2,062 days). Its orbit is tilted by 8 degrees to the plane of the ecliptic and shows an eccentricity of 0.12.

Photometric observations during 2003 showed a rotation period of 17.47±0.05 hours with a brightness variation of 0.50±0.05 in magnitude.[8] The period has since been confirmed by an additional observation.[9] According to the surveys carried out by the Infrared Astronomical Satellite, IRAS, the Japanese Akari satellite, and the U.S. Wide-field Infrared Survey Explorer with its subsequent NEOWISE mission, the asteroid's surface has a very low albedo between 0.03 and 0.05 and a diameter estimate that varies between 55 and 68 kilometers.[4][5][6][7]

The minor planet was named for the ancient Roman town, Aguntum, in the Noricum province of the Roman Empire, in what is nowadays mostly Austria. The naming information was given by the discoverer's widow, who was also the daughter of prolific astronomer Johann Palisa. The historic ruins are located close to Lienz in East Tyrol, the home town of the discoverer.[2] In 1912, shortly before the minor planet's discovery, extensive excavations took place at the Roman site which unearthed coins, pottery masks, bronze objects, and painted tombstones.

References

  1. ↑ 1.0 1.1 1.2 1.3 1.4 "JPL Small-Body Database Browser: 744 Aguntina (1913 QW)". Jet Propulsion Laboratory. https://ssd.jpl.nasa.gov/sbdb.cgi?sstr=2000744. 
  2. ↑ 2.0 2.1 Schmadel, Lutz D. (2003). "(744) Aguntina". Dictionary of Minor Planet Names – (744) Aguntina. Springer Berlin Heidelberg. p. 71. doi:10.1007/978-3-540-29925-7_745. ISBN 978-3-540-29925-7. 
  3. ↑ 3.0 3.1 "LCDB Data for (744) Aguntina". Asteroid Lightcurve Database (LCDB). http://www.minorplanet.info/PHP/generateOneAsteroidInfo.php?AstInfo=744%7CAguntina. 
  4. ↑ 4.0 4.1 4.2 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 22 October 2019. 
  5. ↑ 5.0 5.1 5.2 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)
  6. ↑ 6.0 6.1 6.2 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. doi:10.1088/0004-637X/741/2/90. Bibcode: 2011ApJ...741...90M. http://adsabs.harvard.edu/cgi-bin/bib_query?bibcode=2011ApJ...741...90M. Retrieved 4 January 2016. 
  7. ↑ 7.0 7.1 7.2 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 4 January 2016. 
  8. ↑ 8.0 8.1 Cooney, Walter R. Jr. (March 2005). "Lightcurve results for minor planets 228 Agathe, 297 Caecilia, 744 Aguntina 1062 Ljuba, 1605 Milankovitch, and 3125 Hay". The Minor Planet Bulletin 32 (1): 15–16. ISSN 1052-8091. Bibcode: 2005MPBu...32...15C. http://adsabs.harvard.edu/cgi-bin/bib_query?bibcode=2005MPBu...32...15C. Retrieved 4 January 2016. 
  9. ↑ 9.0 9.1 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 4 January 2016. 
  10. ↑ "744 Aguntina (1913 QW)". Minor Planet Center. https://www.minorplanetcenter.net/db_search/show_object?object_id=744. 

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