Astronomy:1570 Brunonia

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1570 Brunonia
Discovery[1]
Discovered byS. Arend
Discovery siteUccle Obs.
Discovery date9 October 1948
Designations
(1570) Brunonia
Named afterBrown University[2][3]
1948 TX · 1952 QE1
Minor planet categorymain-belt[1][4] · (outer)
Koronis[5][6][7]
Orbital characteristics[4]
Epoch 27 April 2019 (JD 2458600.5)
Uncertainty parameter 0
Observation arc69.89 yr (25,529 d)
|{{{apsis}}}|helion}}3.0028 AU
|{{{apsis}}}|helion}}2.6888 AU
2.8458 AU
Eccentricity0.0552
Orbital period4.80 yr (1,754 d)
Mean anomaly222.99°
Mean motion0° 12m 19.08s / day
Inclination1.6659°
Longitude of ascending node190.05°
226.15°
Physical characteristics
Mean diameter10.80±1.03 km[8]
12.118±0.272 km[9][10]
12.728±0.058 km[11]
Rotation period48 h (or longer)[12]
Geometric albedo0.166[8]
0.169±0.019[13]
0.1909[11]
0.209[9]
S (SDSS-MOC)[14]
Absolute magnitude (H)11.90[9][11]
12.0[1][4][7]
12.40[8]


1570 Brunonia, provisional designation 1948 TX, is a stony asteroid of the Koronis family from the outer regions of the asteroid belt, approximately 12 kilometers (7.5 miles) in diameter. It was discovered on 9 October 1948, by Belgian astronomer Sylvain Arend at the Royal Observatory of Belgium in Uccle.[1] The S-type asteroid is likely elongated and has a longer-than-average rotation period of more than 48 hours.[7] It was named for Brown University in Rhode Island, United States.[2]

Orbit and classification

Brunonia is a core member of the Koronis family (605),[5][6] a very large outer asteroid family with nearly co-planar ecliptical orbits.[7][15] It orbits the Sun in the outer main-belt at a distance of 2.7–3.0 AU once every 4 years and 10 months (1,754 days; semi-major axis of 2.85 AU). Its orbit has an eccentricity of 0.06 and an inclination of 2° with respect to the ecliptic.[4] The body's observation arc begins at Uccle in November 1948, one month after its official discovery observation.[1]

Naming

This minor planet was named for Brown University in Providence, Rhode Island. The 7th oldest university in the United States, Brown was chartered in 1764.[1] The official naming citation was published by the Minor Planet Center in February 1954 (M.P.C. 1040).[16][3]

Physical characteristics

In the SDSS-based taxonomy, Brunonia is a common, stony S-type asteroid,[14] which agrees with the overall spectral type for members of the Koronis family.[15]:23

Rotation period

In February 2016, a rotational lightcurve of Brunonia was obtained from photometric observations by the Kepler spacecraft and its K2 mission (Uranus Field). Lightcurve analysis gave a rotation period of at least 48 hours with a brightness amplitude of more than 0.6 magnitude ({{{1}}}), indicative of an elongated, non-spherical shape.[7][12]

Diameter and albedo

According to the surveys carried out by the Japanese Akari satellite and the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer, Brunonia measures between 10.8 and 12.7 kilometers in diameter and its surface has an albedo between 0.166 and 0.209.[8][9][10][11][13] The Collaborative Asteroid Lightcurve Link assumes an albedo of 0.24 and a diameter of 10.8 kilometers based on an absolute magnitude of 12.0.[7]

References

  1. ↑ 1.0 1.1 1.2 1.3 1.4 1.5 "1570 Brunonia (1948 TX)". Minor Planet Center. https://www.minorplanetcenter.net/db_search/show_object?object_id=1570. Retrieved 11 December 2018. 
  2. ↑ 2.0 2.1 Schmadel, Lutz D. (2007). "(1570) Brunonia". Dictionary of Minor Planet Names. Springer Berlin Heidelberg. p. 124. doi:10.1007/978-3-540-29925-7_1571. ISBN 978-3-540-00238-3. 
  3. ↑ 3.0 3.1 Mitchell, Martha (1993). "Brown University Glacier". Encyclopedia Brunoniana. Providence, RI: Brown University Library. https://www.brown.edu/Administration/News_Bureau/Databases/Encyclopedia/search.php?serial=B0540. Retrieved 11 December 2018. 
  4. ↑ 4.0 4.1 4.2 4.3 "JPL Small-Body Database Browser: 1570 Brunonia (1948 TX)". Jet Propulsion Laboratory. https://ssd.jpl.nasa.gov/sbdb.cgi?sstr=2001570. Retrieved 11 December 2018. 
  5. ↑ 5.0 5.1 "Asteroid 1570 Brunonia". Small Bodies Data Ferret. https://sbntools.psi.edu/ferret/SimpleSearch/results.action?targetName=1570+Brunonia. Retrieved 11 December 2018. 
  6. ↑ 6.0 6.1 "Asteroid (1570) Brunonia – Proper elements". AstDyS-2, Asteroids – Dynamic Site. https://newton.spacedys.com/astdys/index.php?n=1570&pc=1.1.6. Retrieved 10 December 2018. 
  7. ↑ 7.0 7.1 7.2 7.3 7.4 7.5 "LCDB Data for (1570) Brunonia". Asteroid Lightcurve Database (LCDB). http://www.minorplanet.info/PHP/generateOneAsteroidInfo.php?AstInfo=1570%7CBrunonia. Retrieved 11 December 2018. 
  8. ↑ 8.0 8.1 8.2 8.3 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 9.3 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: EAR–A–COMPIL–5–NEOWISEDIAM–V1.0. Bibcode: 2016PDSS..247.....M. https://sbnarchive.psi.edu/pds3/non_mission/EAR_A_COMPIL_5_NEOWISEDIAM_V1_0/data/neowise_mainbelt.tab. Retrieved 11 December 2018. 
  10. ↑ 10.0 10.1 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. 
  11. ↑ 11.0 11.1 11.2 11.3 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.  (catalog)
  12. ↑ 12.0 12.1 Molnár, L.; Pál, A.; Sárneczky, K.; Szabó, R.; Vinkó, J.; Szabó, Gy. M. et al. (February 2018). "Main-belt Asteroids in the K2 Uranus Field". The Astrophysical Journal Supplement Series 234 (2): 10. doi:10.3847/1538-4365/aaa1a1. Bibcode: 2018ApJS..234...37M. 
  13. ↑ 13.0 13.1 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. 
  14. ↑ 14.0 14.1 Carvano, J. M.; Hasselmann, P. H.; Lazzaro, D.; Mothé-Diniz, T. (February 2010). "SDSS-based taxonomic classification and orbital distribution of main belt asteroids". Astronomy and Astrophysics 510: 12. doi:10.1051/0004-6361/200913322. Bibcode: 2010A&A...510A..43C. https://sbnarchive.psi.edu/pds3/non_mission/EAR_A_I0035_5_SDSSTAX_V1_1/data/sdsstax_ast_table.tab. Retrieved 30 October 2019.  (PDS data set)
  15. ↑ 15.0 15.1 Nesvorný, D.; Broz, M.; Carruba, V. (December 2014). "Identification and Dynamical Properties of Asteroid Families". Asteroids IV. pp. 297–321. doi:10.2458/azu_uapress_9780816532131-ch016. ISBN 9780816532131. Bibcode: 2015aste.book..297N. 
  16. ↑ Schmadel, Lutz D. (2009). "Appendix – Publication Dates of the MPCs". Dictionary of Minor Planet Names – Addendum to Fifth Edition (2006–2008). Springer Berlin Heidelberg. p. 221. doi:10.1007/978-3-642-01965-4. ISBN 978-3-642-01964-7. Bibcode: 2009dmpn.book.....S. https://cds.cern.ch/record/1339661. 

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