2009 BD

2009 BD is a micro-asteroid, classified as near-Earth object of the Apollo group and as an Earth co-orbital asteroid.

2009 BD
Discovery[1]
Discovered byMount Lemmon Survey
Discovery siteCatalina Mountains north of Tucson, Arizona, USA
Discovery dateJanuary 16, 2009
Designations
Designation
2009 BD
MPO 201128
NEO · Apollo
Orbital characteristics[2]
Epoch 4 January 2010 (JD 2455200.5)
Uncertainty parameter 0
Observation arc885 days (2.42 yr)
Aphelion1.04978332 AU (157.045349 Gm)
Perihelion0.96744466 AU (144.727661 Gm)
1.00861399 AU (150.886505 Gm)
Eccentricity0.04081772
1.01 yr (369.99 d)
294.29542°
0° 58m 22.83s /day
Inclination0.38516430°
58.487991°
110.50392°
Earth MOID0.00356514 AU (533,337 km)
Physical characteristics
Dimensions7–15 m[3]
Mean density
∼640 kg/m3 [4]
28.1[2]
28.43 ± 0.12[4]

    Orbit

    During the 2011 opposition, the last opposition of 2009 BD that was observed, 2009 BD approached on June 2, 2011 within 0.00231 AU (346,000 km) of the Earth, which is less than 1 lunar distance. For comparison, the distance to the Moon is about 0.0026 AU (384,400 km).

    With an orbital period of 369.99 days, 2009 BD is in a near 1:1 orbital resonance with Earth, and also has about the same orbit around the Sun as Earth. Other resonant near-Earth objects in addition to 2009 BD include 3753 Cruithne (the first to be discovered), (85770) 1998 UP1, 54509 YORP, 2001 GO2, 2002 AA29, 2003 YN107, (164207) 2004 GU9, and 2010 TK7 (an Earth trojan).

    The Jupiter Tisserand invariant, used to distinguish different kinds of orbits, is 6.039.[2] The orbit has a small inclination of about 0.4 degrees.

    JPL[2] and MPC[1] give different parameters for the orbit of 2009 BD, affecting whether the orbit type should be considered an Apollo asteroid or an Amor asteroid. JPL includes non-gravitational acceleration parameters in the orbital solution.

    Physical characteristics

    Because 2009 BD is a very small multi-opposition near-Earth object, the effect of radiation pressure on the orbit caused by light from the Sun was able to be detected.[4] The radiation-related acceleration allowed the Area to Mass Ratio (AMR) to be estimated at (2.97 ± 0.33) × 10−4 m2/kg. Assuming an albedo of 0.12, a typical average for asteroids in the inner solar system, this AMR corresponds to a density of about 640 kg/m3. This density is consistent with the density of very porous rock. For comparison, the asteroid 2006 RH120 has a measured density of about 400 kg/m3, and the density of the asteroid 253 Mathilde as measured by the NEAR-Shoemaker space probe was 1300 kg/m3. In contrast, the density of the man-made near-Earth object 6Q0B44E is 15 kg/m3.

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    gollark: Actually, just do it entirely randomly.
    gollark: If you're just trying to make it even more annoying and complex, why not use... `sin(tan(x))` or something ridiculous like that?
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    gollark: ???

    References
    1. "2009 BD". Minor Planet Center. 20 June 2011.
    2. "JPL Small-Body Database Browser: (2009 BD)" (last observation: 2011-06-20; arc: 885 days). Jet Propulsion Laboratory. Retrieved 30 March 2016.
    3. "ABSOLUTE MAGNITUDE (H)". NASA.
    4. Micheli, Marco; Tholen, David J.; Elliott, Garrett T. (2012). "Detection of radiation pressure acting on 2009 BD". New Astronomy. 17 (4): 446. arXiv:1106.0564. Bibcode:2012NewA...17..446M. doi:10.1016/j.newast.2011.11.008.

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