| Minorplanet: | yes |
| Background: |
|
| Discoverer: | R. S. McMillan Kitt Peak (691) |
| Discovered: | 28 December 2005 |
| Epoch: | 13 January 2016 (JD 2457400.5) |
| Aphelion: | 1.65562913abbr=onNaNabbr=on |
| Perihelion: | 0.659003712AU |
| Semimajor: | 1.15731642AU |
| Eccentricity: | 0.430576028 |
| Period: | 1.25 Jyr (454.75 d) |
| Inclination: | 0.340553512° |
| Asc Node: | 35.9073158° |
| Mean Anomaly: | 175.227687° |
| Arg Peri: | 273.628156° |
| Moid: | 0.000433476AU (0.17 LD) |
| Venus Moid: | 0.0017 AU (0.66 LD) |
| Mars Moid: | 0.03884 AU (15.11 LD) |
| Satellites: | none |
| Spectral Type: | C-type |
| Abs Magnitude: | 21.9 |
| Mean Motion: | / day |
| Rotation: | 18abbr=onNaNabbr=on |
| Mean Radius: | 0.2 km |
| Observation Arc: | 2,183 days (5.98 yr) |
| Uncertainty: | 0 |
| Jupiter Moid: | 3.60813AU |
| Tisserand: | 5.347 |
, provisionally named 2005 YU, is a potentially hazardous asteroid meters in diameter, as measured after its Earth flyby. Previously it was estimated to be 310 meters[1] or about 400 m (1,300 feet) in diameter. It was discovered on 28 December 2005 by Robert S. McMillan at Steward Observatory, Kitt Peak. On 8 November 2011 it passed 0.85 lunar distances (324,900 kilometers; 201,900 miles) from Earth.
In February 2010, was rated 1 on the Torino Scale for a potential pass near Earth on 10 November 2103, that posed no unusual level of danger. On 19 April 2010, radar ranging by the Arecibo radio telescope reduced uncertainties about the orbit by 50%. This improvement eliminated any possibility of an impact with Earth within the next 100 years. It was removed from the Sentry Risk Table on 22 April 2010 and as such it now has a rating of 0 on the Torino Scale. It is now known that on 10 November 2103 will be roughly 2 AU from Earth.
On 8 November 2011 at 23:28 UT the asteroid passed 0.85abbr=onNaNabbr=on from Earth. On 9 November 2011 at 07:13 UT the asteroid passed 0.6231LD from the Moon. During the close approach the asteroid reached about apparent magnitude 11, and would have been visible to experienced observers using high-end binoculars with an objective lens of 80 mm if it were not for bright moonlight preventing a true dark sky. Since the gibbous moon did interfere with the viewing, observers trying to visually locate the asteroid required a telescope with an aperture of 6 inches (15 centimeters) or larger.
The next few times a known asteroid this large will come this close to Earth will be in 2028 when passes 0.65 LD from Earth, and in 2029 when the 325-meter 99942 Apophis comes even closer at just 0.10 LD.[2]
According to Jay Melosh, if an asteroid the size of (~400 m across) were to hit land, it would create a crater 6.3km (03.9miles) across, 518m (1,699feet) deep and generate a seven-magnitude-equivalent-earthquake. The chances of an actual collision with an asteroid like is about 1 percent in the next thousand years.
During the 2011 passage was studied with radar using Goldstone, Arecibo, the Very Long Baseline Array, and the Green Bank Telescope. The Herschel Space Observatory has made far-infrared measurements of on 10 November, helping determine its temperature and composition.
Radar analysis has also helped to pin down the asteroid's albedo, or diffuse reflectivity. Although radar measurements do not detect visible light they can determine the distance and size of an object with a high degree of accuracy. This information, coupled with visible light measurements, provides a more accurate measure of an object's absolute magnitude, and therefore its albedo.
On 8 November 2011, NASA released a statement mentioning a number of structures on the surface of the asteroid, which were detected as it passed near Earth.[3] On 11 November 2011, higher-resolution images showed concavities, a ridge near the asteroid's equator, and numerous features interpreted as decameter-scale boulders. Shape modeling based on the radar images shows that YU55's shape is close to spheroidal, with maximum dimensions of 360±40 m, and an equator-aligned ridge. A 150–200 meter-long, ~20 meter-high rise forms a portion of the ridge-line, and the number of boulders on the surface is comparable to that seen on the asteroid 25143 Itokawa by the Hayabusa spacecraft.
Optical lightcurve measurements during the flyby provided a more accurate estimate of the asteroid's spin period about 19.3 hours. Because is so nearly spheroidal, it was not significantly torqued by Earth's tides during the flyby, and there is no evidence of non-principal-axis rotation. Optical, near-infrared, and ultraviolet[4] spectroscopy confirmed that is a C-type asteroid.
On 19 January 2029, will pass 0.0023AU from Venus. The close approach distance to Venus in 2029 will determine how close the asteroid will pass to Earth in 2041. Before the November 2011 observations, the uncertainties in the post-2029 trajectory showed that the asteroid would pass somewhere between 0.002abbr=onNaNabbr=on and 0.3abbr=onNaNabbr=on of Earth in 2041. Radar astrometry in November 2011 clarified the Earth passage in 2041 and beyond. As a result of the November 2011 radar observations, it is now known that will pass between 0.1017abbr=onNaNabbr=on and 0.1020 AU of Earth on 12 November 2041. Using the current uncertainty region integrated until the future, the 2075 approach will be between 0.0013abbr=onNaNabbr=on and 0.0021abbr=onNaNabbr=on.
