3749 Balam

3749 Balam
Discovery [1]
Discovered by E. Bowell
Discovery site Anderson Mesa Stn.
Discovery date 24 January 1982
Designations
MPC designation (3749) Balam
Named after
 David Balam
(Canadian astronomer)[2]
1982 BG1 · 1954 XM
1962 ED · 1974 YO
main-belt · Flora [3]
Orbital characteristics [1]
Epoch 4 September 2017 (JD 2458000.5)
Uncertainty parameter 0
Observation arc 61.66 yr (22,521 days)
Aphelion 2.4818 AU
Perihelion 1.9920 AU
2.2369 AU
Eccentricity 0.1095
3.35 yr (1,222 days)
254.23°
0° 17m 40.56s / day
Inclination 5.3801°
295.71°
173.74°
Known satellites 2 (⌀: 1.66 km; 1.84 km)[4]
Physical characteristics
Dimensions 4.663±0.214[5][6]
4.7±0.5 km[7]
6.36 km (calculated)[3]
7.2 km[8]
Mass (5.09±0.2)×1014 kg[8][9]
Mean density
 2.61±0.45 g/cm³[8][9]
2.80483±0.00002[10]
2.80478±0.00005 h[lower-alpha 1]
2.80490±0.00008 h[11]
2.80494±0.00007 h[12]
0.15 (assumed)[3]
0.16[13]
0.277±0.096[7]
0.355±0.067[5][6]
S [3][13]
13.3[1] · 13.4[5] · 13.48[14] · 13.66[3][7][11][lower-alpha 1]

    3749 Balam, provisionally known as 1982 BG1, is a stony Florian asteroid and rare trinary system orbiting in the inner regions of asteroid belt.

    It was discovered on 24 January 1982, by American astronomer Edward Bowell at Lowell's Anderson Mesa Station near Flagstaff, Arizona, and named after Canadian astronomer David Balam.[15] Balam measures approximately 5 kilometers in diameter. Its two minor-planet moons have an estimated diameter of 1.66 and 1.84 kilometers, respectively.

    Orbit and classification

    Balam is a member of the Flora family, a very large group of stony asteroids in the inner main-belt. It orbits the Sun in the inner main-belt at a distance of 2.0–2.5 AU once every 3 years and 4 months (1,222 days). Its orbit has an eccentricity of 0.11 and an inclination of 5° with respect to the ecliptic.[1]

    Physical characteristics

    The S-type asteroid has an albedo of 0.16.[13] The body's rotation around its axis has been measured several times by different lightcurve observations with a concurring period of 2.8 hours.[10][11][12][lower-alpha 1]

    Trinary asteroid

    Outer satellite

    On 13 February 2002, the discovery of a minor-planet moon, provisionally designated S/2002 (3749) 1, was announced by a team of researchers from SwRI, UA, JPL and OSUG, using the Gemini North Telescope on Mauna Kea in Hawaii.[16] It has an estimated diameter of 1.84 kilometers. It orbits 289±13 km away in 61±10 days, with an orbital eccentricity of ~ 0.9.[9]

    Being such a small primary body in the inner main belt with a separation of over 100 primary radii, S/2002 (3749) 1 is the most loosely bound binary known.[17] Balam has a Hill sphere with a radius of about 1,500 kilometers.[9]

    Inner satellite

    In March 2008, Franck Marchis discovered another companion, provisionally designated S/2008 (3749) 1, making Balam a trinary asteroid.[18][19] The inner satellite has a derived diameter of 1.66 kilometer, based on diameter-ratio of 0.42±0.03 with its primary.[4]

    Other known trinary asteroids include 45 Eugenia, 87 Sylvia, 93 Minerva, 107 Camilla, 130 Elektra and 216 Kleopatra.

    Naming

    It is named after the Canadian astronomer David Balam, principal observer at Victoria's Climenhaga Observatory in British Columbia.[2] The approved naming citation was published by the Minor Planet Center on 31 May 1988 (M.P.C. 13178).[20]

    Notes

    1. 1 2 3 Pravec-2012web, rotation period of 2.80478±0.00005 with an amplitude in brightness variation of 0.1 magnitude. Summary figures for (3749) Balam at Lightcurve Database

    References

    1. 1 2 3 4 "JPL Small-Body Database Browser: 3749 Balam (1982 BG1)" (2016-08-03 last obs.). Jet Propulsion Laboratory. Retrieved 16 June 2017.
    2. 1 2 Schmadel, Lutz D. (2007). Dictionary of Minor Planet Names – (3749) Balam. Springer Berlin Heidelberg. p. 317. ISBN 978-3-540-00238-3. Retrieved 16 June 2017.
    3. 1 2 3 4 5 "LCDB Data for (3749) Balam". Asteroid Lightcurve Database (LCDB). Retrieved 16 June 2017.
    4. 1 2 Wm. Robert Johnston (2009-01-13). "(3749) Balam, S/2002 (3749) 1, and third component". Johnston's Archive. Retrieved 27 October 2009.
    5. 1 2 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. arXiv:1109.6407. Bibcode:2011ApJ...741...90M. doi:10.1088/0004-637X/741/2/90. Retrieved 11 November 2015.
    6. 1 2 Masiero, Joseph R.; Mainzer, A. K.; Grav, T.; Bauer, J. M.; Cutri, R. M.; Dailey, J.; et al. (November 2011). "Main Belt Asteroids with WISE/NEOWISE. I. Preliminary Albedos and Diameters". The Astrophysical Journal. 741 (2): 20. arXiv:1109.4096. Bibcode:2011ApJ...741...68M. doi:10.1088/0004-637X/741/2/68. Retrieved 16 June 2017.
    7. 1 2 3 Marchis, F.; Enriquez, J. E.; Emery, J. P.; Mueller, M.; Baek, M.; Pollock, J.; et al. (November 2012). "Multiple asteroid systems: Dimensions and thermal properties from Spitzer Space Telescope and ground-based observations". Icarus. 221 (2): 1130–1161. arXiv:1604.05384. Bibcode:2012Icar..221.1130M. doi:10.1016/j.icarus.2012.09.013. Retrieved 11 November 2015.
    8. 1 2 3 Jim Baer (12 December 2010). "Recent Asteroid Mass Determinations". Personal Website. Retrieved 16 June 2017.
    9. 1 2 3 4 Marchis, F.; Descamps, P.; Berthier, J.; Hestroffer, D.; Vachier, F.; Baek, M.; et al. (May 2008). "Main belt binary asteroidal systems with eccentric mutual orbits". Icarus. 195 (1): 295–316. arXiv:0804.1385. Bibcode:2008Icar..195..295M. doi:10.1016/j.icarus.2007.12.010. Retrieved 16 June 2017.
    10. 1 2 Marchis, F.; Pollock, J.; Pravec, P.; Baek, M.; Greene, J.; Hutton, L.; et al. (March 2008). "(3749) Balam". Central Bureau Electronic Telegrams. Bibcode:2008CBET.1297....1M. Retrieved 11 November 2015.
    11. 1 2 3 Polishook, D.; Brosch, N.; Prialnik, D. (March 2011). "Rotation periods of binary asteroids with large separations - Confronting the Escaping Ejecta Binaries model with observations". Icarus. 212 (1): 167–174. arXiv:1012.4810. Bibcode:2011Icar..212..167P. doi:10.1016/j.icarus.2010.12.020. Retrieved 11 November 2015.
    12. 1 2 Polishook, D. (October 2014). "Spin axes and shape models of asteroid pairs: Fingerprints of YORP and a path to the density of rubble piles". Icarus. 241: 79–96. arXiv:1406.3359. Bibcode:2014Icar..241...79P. doi:10.1016/j.icarus.2014.06.018. Retrieved 11 November 2015.
    13. 1 2 3 Thomas Wm Hamilton. "Dwarf Planets and Asteroids: Minor Bodies of the Solar System".
    14. ↑ Veres, Peter; Jedicke, Robert; Fitzsimmons, Alan; Denneau, Larry; Granvik, Mikael; Bolin, Bryce; et al. (November 2015). "Absolute magnitudes and slope parameters for 250,000 asteroids observed by Pan-STARRS PS1 - Preliminary results". Icarus. 261: 34–47. arXiv:1506.00762. Bibcode:2015Icar..261...34V. doi:10.1016/j.icarus.2015.08.007. Retrieved 16 June 2017.
    15. ↑ "3749 Balam (1982 BG1)". Minor Planet Center. Retrieved 11 November 2015.
    16. ↑ "IAUC 7827: P/2001 WF_2; S/2002 (3749) 1". IAU Central Bureau for Astronomical Telegrams. 2002-02-13. Retrieved 17 November 2005.
    17. ↑ Merline, W. J.; Close, L. M.; Siegler, N.; Dumas, C.; Chapman, C. R.; Rigaut, F.; et al. (September 2002). "Discovery of a Loosely-bound Companion to Main-belt Asteroid (3749) Balam". American Astronomical Society. 34: 835. Bibcode:2002DPS....34.0201M. Retrieved 16 June 2017.
    18. ↑ "IAUC 8928: V2468 Cyg = N Cyg 2008; (3749)". IAU Central Bureau for Astronomical Telegrams. 2008-03-19. Retrieved 4 February 2012.
    19. ↑ Franck Marchis (Principal Investigator, SETI Institute, UC Berkeley). "Franck Marchis Web Page". Department of Astronomy (University of California at Berkeley). Archived from the original on 2007-11-10. Retrieved 2009-10-27.
    20. ↑ "MPC/MPO/MPS Archive". Minor Planet Center. Retrieved 16 June 2017.
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