1729 Beryl
Discovery[1]
Discovered byIndiana University
(Indiana Asteroid Program)
Discovery siteGoethe Link Obs.
Discovery date19 September 1963
Designations
(1729) Beryl
Named after
Beryl H. Potter[2]
(research assistant)
1963 SL · 1933 ST
1942 EW · 1949 JL
1950 VR · 1952 DO2
1955 BD · 1959 JB
1959 JL · 1959 LH
1972 GD2
main-belt[1][3] · (inner)
background[4][5]
Orbital characteristics[3]
Epoch 27 April 2019 (JD 2458600.5)
Uncertainty parameter 0
Observation arc84.59 yr (30,896 d)
Aphelion2.4548 AU
Perihelion2.0049 AU
2.2299 AU
Eccentricity0.1009
3.33 yr (1,216 d)
328.58°
0° 17m 45.6s / day
Inclination2.4418°
9.0601°
262.31°
Physical characteristics
Mean diameter
9.037±1.031 km[6][7]
4.8888±0.0003 h[8]
0.246[6][7]
SMASS = S[3][9]
12.130±0.001 (R)[10]
12.36[7]
12.40[6]
12.5[1][3][9]

    1729 Beryl, provisional designation 1963 SL, is a stony background asteroid from the Florian region in the inner asteroid belt, approximately 9 kilometers (5.6 miles) in diameter. It was discovered on 19 September 1963, by astronomers at Indiana University during the Indiana Asteroid Program at Goethe Link Observatory in Indiana, United States.[1] The S-type asteroid has a rotation period of 4.9 hours.[9] It was named for Beryl H. Potter, a long-time research assistant of the discovering program.[2]

    Orbit and classification

    Beryl is a non-family asteroid of the main belt's background population when applying the hierarchical clustering method to its proper orbital elements.[4][5] Based on osculating Keplerian orbital elements, the asteroid has also been classified as a member of the Flora family (402), a giant asteroid family and the largest family of stony asteroids in the main-belt.[9] It orbits the Sun in the inner asteroid belt at a distance of 2.0–2.5 AU once every 3 years and 4 months (1,216 days; semi-major axis of 2.23 AU). Its orbit has an eccentricity of 0.10 and an inclination of 2° with respect to the ecliptic.[3]

    The asteroid was first observed as 1933 ST at Simeiz Observatory in September 1933. The body's observation arc begins with its observation as 1942 EW at Turku Observatory in March 1942, or more than 21 years prior to its official discovery observation at Goethe Link.[1]

    Naming

    This minor planet was named after Beryl H. Potter (1900–1985), research assistant at the Indiana University, who participated in the program of minor planet observations from 1949 to 1966. During this period, she analysed nearly 6,300 photographic plates, measuring the positions of minor planets and reporting lost asteroids to the International Astronomical Union, which were then published in the Minor Planet Circulars.[2][11] The official naming citation was published by the Minor Planet Center on 15 July 1968 (M.P.C. 2883).[12]

    Physical characteristics

    In the SMASS classification, Beryl is a common, stony S-type asteroid.[4][9]

    Rotation period

    In May 2009, a rotational lightcurve of Beryl was obtained from photometric observations by Julian Oey at the Leura (E17) and Kingsgrove (E19) observatories in Australia. Lightcurve analysis gave a rotation period of 4.8888±0.0003 hours and a brightness variation of 0.20 magnitude (U=3).[8] In addition, a nearly identical period of 4.889±0.0014 hours with an amplitude of 0.14 was determined in the R-band by astronomers at the Palomar Transient Factory in October 2010 (U=2).[10]

    Diameter and albedo

    According to the survey carried out by the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer, Beryl measures 9.04 kilometers in diameter and its surface has an albedo of 0.246.[6][7] The Collaborative Asteroid Lightcurve Link assumes an albedo of 0.24 – derived from 8 Flora, the namesake of the Flora Family – and calculates a diameter of 8.58 kilometers based on an absolute magnitude of 12.5.[9]

    References

    1. 1 2 3 4 5 "1729 Beryl (1963 SL)". Minor Planet Center. Retrieved 10 December 2018.
    2. 1 2 3 Schmadel, Lutz D. (2007). "(1729) Beryl". Dictionary of Minor Planet Names – (1729) Beryl. Springer Berlin Heidelberg. p. 137. doi:10.1007/978-3-540-29925-7_1730. ISBN 978-3-540-00238-3.
    3. 1 2 3 4 5 "JPL Small-Body Database Browser: 1729 Beryl (1963 SL)" (2018-04-23 last obs.). Jet Propulsion Laboratory. Retrieved 10 December 2018.
    4. 1 2 3 "Asteroid 1729 Beryl". Small Bodies Data Ferret. Retrieved 10 December 2018.
    5. 1 2 "Asteroid (1729) Beryl – Proper elements". AstDyS-2, Asteroids – Dynamic Site. Retrieved 10 December 2018.
    6. 1 2 3 4 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 10 December 2018.
    7. 1 2 3 4 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.
    8. 1 2 Oey, Julian (October 2010). "Light Curve Analysis of Asteroids from Leura and Kingsgrove Observatory in the First Half of 2009". The Minor Planet Bulletin. 37 (4): 135–136. Bibcode:2010MPBu...37..135O. ISSN 1052-8091. Retrieved 10 December 2018.
    9. 1 2 3 4 5 6 "LCDB Data for (1729) Beryl". Asteroid Lightcurve Database (LCDB). Retrieved 10 December 2018.
    10. 1 2 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:1504.04041. Bibcode:2015AJ....150...75W. doi:10.1088/0004-6256/150/3/75.
    11. ↑ "Beryl Potter". Physics Today. 39 (2): 92. February 1986. doi:10.1063/1.2814912.
    12. ↑ Schmadel, Lutz D. "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.
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