1570 Brunonia

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1570 Brunonia
Discovery [1]
Discovered by S. Arend
Discovery site Uccle Obs.
Discovery date9 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
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]

    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]

    Contents

    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 space telescope 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

    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]

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    References

    1. 1 2 3 4 5 6 "1570 Brunonia (1948 TX)". Minor Planet Center. Retrieved 11 December 2018.
    2. 1 2 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. 1 2 Mitchell, Martha (1993). "Brown University Glacier". Encyclopedia Brunoniana. Providence, RI: Brown University Library. ASIN   B0006P9F3C . Retrieved 11 December 2018.
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    7. 1 2 3 4 5 6 "LCDB Data for (1570) Brunonia". Asteroid Lightcurve Database (LCDB). Retrieved 11 December 2018.
    8. 1 2 3 4 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)
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    13. 1 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. arXiv: 1209.5794 . Bibcode:2012ApJ...759L...8M. doi:10.1088/2041-8205/759/1/L8. S2CID   46350317.
    14. 1 2 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)
    15. 1 2 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.
    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. Bibcode:2009dmpn.book.....S. doi:10.1007/978-3-642-01965-4. ISBN   978-3-642-01964-7.
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