| Minorplanet: | yes |
| 3749 Balam | |
| Background: |
|
| Discovery Ref: |   |
| Discovered: | 24 January 1982 |
| Mpc Name: | (3749) Balam |
| Alt Names: | 1954 XM 1962 ED1974 YO |
| Named After: | David Balam |
| Mp Category: | main-beltFlora  |
| Orbit Ref: |   |
| Epoch: | 4 September 2017 (JD 2458000.5) |
| Uncertainty: | 0 |
| Observation Arc: | 61.66 yr (22,521 days) |
| Perihelion: | 1.9920 AU |
| Semimajor: | 2.2369 AU |
| Eccentricity: | 0.1095 |
| Period: | 3.35 yr (1,222 days) |
| Mean Motion: | / day |
| Inclination: | 5.3801° |
| Asc Node: | 295.71° |
| Arg Peri: | 173.74° |
| Satellites: | 2 |
| Mean Diameter: | |
| Albedo: | 0.16 |
| Spectral Type: | Sq  |
| Abs Magnitude: | 13.3 13.4 13.66 |
3749 Balam is a stony Flora asteroid and rare trinary system orbiting in the inner regions of asteroid belt. It also forms a secured asteroid pair with sub-kilometer sized asteroid . Balam was discovered on 24 January 1982, by American astronomer Edward Bowell at Lowell's Anderson Mesa Station near Flagstaff, Arizona, and received the prov. designation . It was named after Canadian astronomer David Balam. Balam measures approximately 4.1km (02.5miles) in diameter. Its two minor-planet moons have an estimated diameter of 1.66 and 1.84 kilometers, respectively.
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.
It is named after the Canadian astronomer David Balam, principal observer at Victoria's Climenhaga Observatory in British Columbia. The approved naming citation was published by the Minor Planet Center on 31 May 1988 .
The S-type asteroid has an albedo of 0.16. The body's rotation around its axis has been measured several times by different lightcurve observations with a concurring period of 2.8 hours.
On 13 February 2002, the discovery of a minor-planet moon, provisionally designated, was announced by a team of researchers from SwRI, UA, JPL and OSUG, using the Gemini North Telescope on Mauna Kea in Hawaii. It has an estimated diameter of 1.84 kilometers. It orbits km away in days, with a high orbital eccentricity of ~ 0.9. The distant and highly eccentric orbit of S/2002 (3749) 1 suggests that it was likely captured by Balam.
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. Balam has a Hill sphere with a radius of about 1,500 kilometers.
In March 2008, Franck Marchis discovered another companion, provisionally designated, making Balam a trinary asteroid. The inner satellite has a derived diameter of 1.66 kilometer, based on diameter-ratio of with its primary.
Other known trinary asteroids include 45 Eugenia, 87 Sylvia, 93 Minerva, 107 Camilla, 130 Elektra and 216 Kleopatra.
Balam also forms an asteroid pair with . Asteroid pairs are on highly similar heliocentric orbits. At some point in the past, the pair of asteroids became gravitationally unbound due to rotational fission induced by the YORP-effect or from a collisional breakup of the parent body. After the discovery of Balams two satellites by Bill Merline (inner moon) and Franck Marchis (outer moon) in 2002 and 2008, respectively, Czech physicist David Vokrouhlický identified the unbound secondary in 2009. Based on backward orbit integrations, it is thought that Balam and form a secured asteroid pair that became separated approximately 400,000 years ago.