1570 Brunonia
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]
| Discovery[1] | |
|---|---|
| Discovered by | S. Arend |
| Discovery site | Uccle Obs. |
| Discovery date | 9 October 1948 |
| Designations | |
| (1570) Brunonia | |
Named after | Brown University[2][3] |
| 1948 TX · 1952 QE1 | |
| main-belt[1][4] · (outer) Koronis[5][6][7] | |
| Orbital characteristics[4] | |
| Epoch 27 April 2019 (JD 2458600.5) | |
| Uncertainty parameter 0 | |
| Observation arc | 69.89 yr (25,529 d) |
| Aphelion | 3.0028 AU |
| Perihelion | 2.6888 AU |
| 2.8458 AU | |
| Eccentricity | 0.0552 |
| 4.80 yr (1,754 d) | |
| 222.99° | |
| 0° 12m 19.08s / day | |
| Inclination | 1.6659° |
| 190.05° | |
| 226.15° | |
| Physical characteristics | |
Mean diameter | 10.80±1.03 km[8] 12.118±0.272 km[9][10] 12.728±0.058 km[11] |
| 48 h (or longer)[12] | |
| 0.166[8] 0.169±0.019[13] 0.1909[11] 0.209[9] | |
| S (SDSS-MOC)[14] | |
| 11.90[9][11] 12.0[1][4][7] 12.40[8] | |
Orbit and classification edit
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 edit
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 edit
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 edit
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 (U=n.a.), indicative of an elongated, non-spherical shape.[7][12]
Diameter and albedo edit
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 edit
- ^ a b c d e f "1570 Brunonia (1948 TX)". Minor Planet Center. Retrieved 11 December 2018.
- ^ a b 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.
- ^ a b Mitchell, Martha (1993). "Brown University Glacier". Encyclopedia Brunoniana. Providence, RI: Brown University Library. ASIN B0006P9F3C. Retrieved 11 December 2018.
- ^ a b c d "JPL Small-Body Database Browser: 1570 Brunonia (1948 TX)" (2018-09-01 last obs.). Jet Propulsion Laboratory. Retrieved 11 December 2018.
- ^ a b "Asteroid 1570 Brunonia". Small Bodies Data Ferret. Retrieved 11 December 2018.
- ^ a b "Asteroid (1570) Brunonia – Proper elements". AstDyS-2, Asteroids – Dynamic Site. Retrieved 10 December 2018.
- ^ a b c d e f "LCDB Data for (1570) Brunonia". Asteroid Lightcurve Database (LCDB). Retrieved 11 December 2018.
- ^ 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. (online, AcuA catalog p. 153)
- ^ a b c d 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. Retrieved 11 December 2018.
- ^ a b 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. S2CID 119293330.
- ^ a b c d 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. S2CID 35447010. (catalog)
- ^ a b 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. arXiv:1706.06056. Bibcode:2018ApJS..234...37M. doi:10.3847/1538-4365/aaa1a1. S2CID 119423034.
- ^ a b 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. arXiv:1209.5794. Bibcode:2012ApJ...759L...8M. doi:10.1088/2041-8205/759/1/L8. S2CID 46350317.
- ^ a b 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. Bibcode:2010A&A...510A..43C. doi:10.1051/0004-6361/200913322. Retrieved 30 October 2019. (PDS data set)
- ^ a b Nesvorný, D.; Broz, M.; Carruba, V. (December 2014). "Identification and Dynamical Properties of Asteroid Families". Asteroids IV. pp. 297–321. arXiv:1502.01628. Bibcode:2015aste.book..297N. doi:10.2458/azu_uapress_9780816532131-ch016. ISBN 9780816532131. S2CID 119280014.
- ^ 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. Bibcode:2009dmpn.book.....S. doi:10.1007/978-3-642-01965-4. ISBN 978-3-642-01964-7.
External links edit
- Asteroid Lightcurve Database (LCDB), query form (info 16 December 2017 at the Wayback Machine)
- Dictionary of Minor Planet Names, Google books
- Discovery Circumstances: Numbered Minor Planets (1)-(5000) – Minor Planet Center
- 1570 Brunonia at AstDyS-2, Asteroids—Dynamic Site
- Ephemeris · Observation prediction · Orbital info · Proper elements · Observational info
- 1570 Brunonia at the JPL Small-Body Database